nal Bureau of Standards

"• Library, M.W. Bldg ^

MAY 1 1963

^ecknical vtote 171

BIBLIOGRAPHY ON ATMOSPHERIC

ASPECTS OF RADIO ASTRONOMY

Including Selected References to Related Fields

WILHELM NUPEN

U. S. DEPARTMENT OF COMMERCE

NATIONAL BUREAU OF STANDARDS
THE NATIONAL BUREAU OF STANDARDS

Functions and Activities

The functions of the National Bureau of Standards are set forth in the Act of Congress,

March 3, 1901, as amended by Congress in Public Law 619, 1950. These include the development and maintenance of the national standards of measurement and the provision of means

and methods for making measurements consistent with these standards; the determination of physical constants and properties of materials; the development of methods and instruments

for testing materials, devices^ and structures; advisory services to government agencies on

scientific and technical problems; invention and development of devices to serve special needs

of the Government; and the development of standard practices, codes, and specifications. The

work includes basic and applied research, development, engineering, instrumentation, testing,

evaluation, calibration services, and various consultation and information services. Research

projects are also performed for other government agencies when the work relates to and supplements the basic program of the Bureau or when the Bureau's unique competence is required.

The scope of activities is suggested by the listing of divisions and sections on the inside of

the back cover.

Publications

The results of the Bureau's research are published either in the Bureau's own series of

publications or in the journals of professional and scientific societies. -The Bureau publishes

three periodicals available from the Government Printing Office: The Journal of Research,

published in four separate sections, presents complete scientific and technical papers; the Technical News Bulletin presents summary and preliminary reports on work in progress; and the

Central Radio Propagation Laboratory Ionospheric Predic lions provides data for determining

the best frequencies to use for radio communications throughout the world. There are also

five series of nonperiodical publications: Monographs, Applied Mathematics Series, Handbooks,

Miscellaneous Publications, and Technical Notes.

A complete listing of the Bureau's publications can be found in National Bureau of Standards Circular 460, Publications of the National Bureau of Standards, 1901 to June 1947 ($1.25),

and the Supplement to National Bureau of Standards Circular 460, July 1947 to June 1957

($1.50), and Miscellaneous Publication 240, July 1957 to June 1960 (includes Titles of Papers

Published in Outside Journals 1950 to 1959) ($2.25); available from the Superintendent of

Documents, Government Printing Office, Washington 25, D.C.
NATIONAL BUREAU OF STANDARDS

171

ISSUED MAY 1, 1963

BIBLIOGRAPHY ON ATMOSPHERIC ASPECTS

OF RADIO ASTRONOMY

Including Selected References to Related Fields

Wilhelm Nupen

Prepared by

American Meteorological Society

Meteorological & Geoastrophysical Abstracts

NBS Technical Notes are designed to supplement the Bureau's regular publications program. They provide a means for making available scientific data that are of transient or limited interest. Technical Notes may be

listed or referred to in the open literature.

For sale by the Superintendent of Documents, U.S. Government Printing Office Washington 25, D.C. Price ft X. > C^D

CONTENTS

INTRODUCTION Page i

SUBJECT OUTLINE iii

GEOGRAPHIC OUTLINE li

CHRONOLOGICAL INDEX lx

BIBLIOGRAPHY ON ATMOSPHERIC ASPECTS

OF RADIO ASTRONOMY, INCLUDING

SELECTED REFERENCES TO RELATED

FIELDS 1

AUTHOR INDEX 373
Note:

Abstractors/Bibliog. on Atmospheric Aspects of Radio Astronomy

Including Selected References to Related Fields

MGA Staff members:

A. A Andrew Assur

C. E. P. B C. E. P. Brooks

R. B Ronald Baker

K. C Kiwon Chung

E. K Elemer Kiss

D. B. K Dov B. Krimgold

A. J. M Andrew J. Meglis

N. N Nndem E. U. Nndem

S.N Sylvia Nowinska

W. N Wilhelm Nupen

A. M. P Alexis M. Poushkin

M. L. R Mary L. Rice

M. R Malcolm Rigby

I. S Ismael Saad

N. P. S Nicholas P. Setchkin

E. Z. S Evelyn Z. Sinha

G. T Geza Thuronyi

O. T Otto Taborsky

A. V Andre Vandenplas

Others:

1

IRE Absts. (Institute of Radio Engineers, Proceedings)

Bulletin Signaletique Absts.

Elec. Eng. Absts.

Physics Absts.

NASA Absts. (National Aeronautics and Space Administration)

CSIRO (Commonwealth Scientific and Industrial Research

Organization. Div. of Radiophysics, Sydney, Australia)

L. A. Manning

R. S.Quiroz

Library Symbols:

BBS U. S. National Bureau of Standards, Wash. , D. C.

DGS U. S. Geological Survey, Wash. , D. C.

DLC Library of Congress, Wash. , D. C.

DWB U.S. Weather Bureau, Suitland, Maryland

DN-HO U. S. Navy Hydrographic Office, Suitland, Maryland
BIBLIOGRAPHY ON ATMOSPHERIC ASPECTS

OF RADIO ASTRONOMY

INCLUDING SELECTED REFERENCES TO RELATED FIELDS

INTRODUCTION

This is the fourth in a series of bibliographies being prepared by

the M & GA staff of the American Meteorological Society for the

Boulder Laboratories of the National Bureau of Standards. The first

three were:

1. Bibliography on Ionospheric Propagation of

Radio Waves (1923-1960). NBS Technical

Note No. 84, October 1960. (1404 items)

2. Bibliography on Meteoric Radio Wave Propagation. NBS Technical Note No. 94, May

1961. (368 items)

3. Bibliography on Auroral Radio "Wave Propagation. NBS Technical Note No. 128, January

1962. (297 items)

The present bibliography on Atmospheric Aspects of Radio Astronomy Including Selected References to Related Fields contains over a thousand abstracts or titles taken from the literature published between

1900 and 1961, incl. , but the bulk of the literature follows the discovery by Jansky in 1932 of radiofrequency radiation from the sun, and

especially the building of radio telescopes since World War II. The subject matter in this bibliography is confined to the effects

of the Earth's atmosphere on radiofrequency radiation from the sun,

planets, stars, the galaxies and intergalactic space, or knowledge of

atmospheric or ionospheric structure, composition, or physics.

Obviously only a small portion of the vast amount of current and

past literature on radio astronomy is included in the above definition,

yet in spite of this fact, and in spite of serious gaps in the coverage

of the world's literature in this field, the selection of material has
been quite rigorous in order that the volume of material would not get

out of hand.

A small amount of material is included on propagation of radio

waves in or from atmospheres of other planets, or reflections from

these planets. Other borderline aspects of the broad field are also

touched on but not treated exhaustively since the main emphasis is

on the various influences exerted by the Earth's atmosphere on terrestrial or extra-terrestrial radiofrequency radiation.

The following detailed subject outline shows the scope and the

many facets of the material included herein. A geographical, author,

and chronological index are also included.

We wish to express appreciation for guidance given by the staff

of the NBS Boulder Laboratories, particularly to Mr. Bradford R.Bean

for valuable assistance in determining the scope and content of this

and previous bibliographies on radio propagation. We also wish to

thank Mrs. Doris Nickey for patient labor in typing and correcting the

master copy of these four bibliographies, and to other members of the

M&GA staff for their contributions.

The first three bibliographies listed above are available through

the U.S. Department of Commerce, Office of Technical Services, Washington 25, D. C. This new publication, NBS Technical Note No. 171,

is available from the Superintendent of Documents, U.S. Government

Printing Office, Washington 25, D. C.

Supplements to these bibliographies, and a compilation of material on tropospheric propagation of radio waves are in progress.

Any comments, criticisms, corrections, additions, or material

for future radio propagation bibliographies should be addressed to:

Malcolm Rigby, Editor

Meteorological & Geoastrophysical

Abstracts

P. O. Box 1736

Washington 13, D. C.

li
SUBJECT OUTLINE

I. GENERAL WORKS

1. Textbooks, monographs, manuals. D-28, 52, 58, 92, 114, 125,

142, 194, 212, 215, 314, 320, 349, 355, 382, 419, 433,

437, 442, 449, 451, 474, 502, 521, 524, 525, 533, 547,

583, 612, 623, 667, 659, 704, 722, 750, 751, 761, 765,

779, 782, 839, 841

Yearbooks. D-105, 106

Popular science books, etc. D-115, 144, 168, 269, 475, 749,

939

2. General reviews and surveys. D-24, 53, 55, 61, 68, 84, 103,

138, 213, 216, 272, 324, 350, 363, 375, 381, 394, 403,

429, 431, 465, 466, 492, 505, 532, 557, 574, 578, 580,

619, 625, 668, 679, 686, 687, 696, 727, 819, 873, 935,

952, 969, 989, 1006, 1007

Collected works. D-52, 499, 668, 806

lectures. D-84, 218, 477, 546, 665, 1010

3. Data publications. D-4, 17, 18, 51, 53, 105, 106, 148, 180,

225, 234, 278, 285, 358, 567, 648, 727, 754, 802,

930, 989

Scientific reports. D-24, 48, 76, 134, 137, 189, 289, 337,

358, 362, 367, 448, 480, 522, 523, 542, 586, 587, 597,

636, 685, 723, 780, 872, 873, 876, 917

Committee reports. D-l, 15, 22, 44, 184, 273, 301, 330, 331,

346, 368, 428, 548, 568, 570-575, 582, 611, 728, 779,

838

Technical reports. D-516, 714, 823, 969

Statistical data. D-l, 101, 141, 179, 266, 513, 636, 719

Analyses. D-35, 110, 267

Catalogues. D-611, 995, 1009

in
Miscellaneous data

Ballistics D-17

Dawn chorus D-636

Early experimental results D-679

Eclipses D-4, 863

Electron density D-17, 18

Electron density with satellite height D-920

Noise D-llf 15, 329

Project Vanguard D-580

Radars as ionospheric probe D-685, 841

Radio star scintillation D-265

Rocket radio reception D-480

Rockets and satellites/USSR and USA D-754

Satellite break-up D-409

Satellite cloud photography D-1009

Satellite data/cosmic radiation D-427, 584

Satellite-obtained data D-761, 819

Satellite orbit forecasts D-715

Scintillation D-4

Sferics D-567, 591

Shock layer D-224

Short-wave absorption D-891

Signal strength D-257

Solar bursts and flares D-270, 514, 542, 648, 926

Solar radio emission D-328, 567, 579, 714, 899

Upper air wind directions and speed D-940

Whistlers D-554, 567, 636

4. Theses

Ph. D. D-462

5. Maps and nomograms. D-80, 83, 154, 251, 394, 405, 445,

643, 732, 761, 823, 884, 887, 1009

6. Bibliographies (>50refs.) D-16, 52, 92, 105^108, 144, 168,

212, 215, 225, 235, 272, 300, 320, 330, 349, 355, 358,

362, 419, 446, 449, 466, 477, 521, 524, 530, 532, 547,

572-574, 582, 583, 586, 587, 594, 608, 612, 667-669,

706, 714, 727, 751, 836, 839, 841, 866, 938, 946, 960

7. History. D-169, 272, 339-345, 432, 474, 546, 623, 679, 751,

784, 797

8. Conferences, symposia. D-36, 44, 75, 133, 142, 146, 170,

182, 199, 224, 226, 273, 287, 309, 373, 374, 429, 444,

449, 451, 467, 512, 524, 546, 570, 571, 608, 651, 718,

782, 806-808, 868, 929, 945, 957

IV
9. Research programs. D-275, 374, 554, 580, 581, 839, 647,

681, 890, 929, 932, 945, 953, 978

I. G. Y. D-33, 50, 58, 85, 86, 106, 113, 183, 215, 241, 270,

324, 328, 329, 364, 374, 375, 443, 470, 509, 554,

567, 568, 578, 580, 585, 599, 639, 715, 728, 760,

761, 954, 978, 980, 990, 1005

Rocket and satellite programs. D-755, 760, 845, 944, 949,

961, 981

Expeditions. D-387, 704, 734, 802

10. Nomenclature, encyclopedia. D-638, 766, 785, 947

II. THEORIES

Bailey's theory/ non-uniform ionized gas D-195

Bremmer's theory D-128

Chapman's law, modified D-720

Hatanaka's theory/Faraday dispersion D-137, 138

Kraus' hypothesis D-312, 411

Little's diffraction theory D-460

Martyn's theory D-154, 157

Shklovsky's method/distance to source D-988

Stormer's theory, improved version D-590, 592

1. Miscellaneous

Attenuation equivalence theorem D-34

Atmospheric scattering D-69

Ballistic theory D-999

Communication theory D-746

Discrete interval theorem D-83

"Dropout" theory D-473

Earth revolving within solar corona D-13

Eddy current D-907

Effect of planetary positions on SW signals D-576

Electrical field and discharge D-95

Electron scattering, review of theories D-1003

Faraday effects D-160

F-region irregularities D-157

Galactic and solar radiation D-706

Geomagnetism of corpuscular origin D-614

Hypothesis/3. 2 cm radiation and the D layer D-271

Ion circulation in Earth's and Sun's electric fields D-911
Ionospheric absorption D-469

Ionospheric theory D-543

Ionospheric Y-mode propagation, improved theory D-680

Magneto-ionic theory D-176, 532, 667

Moon's quasi-smooth reflection characteristics D-736, 737

Origin of ionospheric irregularities D-156

Penetration of radio waves from space D-128

Perturbation theory D-780

Plasma conductivity D-687

Plasma hypothesis D-905

Radiation (spectra) origin D-335

Radio interferometry D-79

Radio star scintillation D-72

Radio wave propagation in plasma D-634

Radio wave propagation, review of theories D-667

Remote radio navigation and control D-846

Satellite methods/review D-961

Satellite produced ionization D-472

Scintillation D-713

Solar burst type I / review of theories D-975

Solar frequency radiation/thermal theories D-630, 707

Statistical theories, criteria D-746

Statistical theories, starlight intensity D-842

Statistical theories, turbulence D-73

Sunflare emitted protons/ionizing agent D-319

Sunspots D-790

Sunspots, review of theories D-588

Test of the theoretical laws governing frequency dependence

of scintillation, amplitude and rate D-121

Turbulence theory/ionospheric scatter propagation D-889

VLF Emissions from exosphere D-483

VLF mode theory D-591

Whistler origin D-152

Whistler propagation D-152

Whistler trapping D-778

See also: METHODS AND TECHNIQUES OF OBSERVATION

p. xxxx

2. Models

A. R.D. C. atmospheric model D-323

Atmospheric temperature distribution model D-353

Baumbach-AUen model D-690

Collision model D-735

Exosphere/whistlers D-236

Frequency dependence D-625

Gallet's turbulence model D-99

Hard- sphere model D-735

VI
Ionic distribution model/exosphere D-609

Ionization model/satellite surface emission D-519

Ionospheric models D-386

Ionospheric models, density D-531

Ionospheric models, satellite signals D-304, 377

Lunar surface model D-387

Mill's spiral model D-989

Orion nebula D-1000

Parabolic layer model/electron density D-962

Plasma models D-288, 401, 493

Solar models D-250, S28, 707, 911

Solution of propagation of discrete radio noise sources D-872

3. Formulas

Allen - Baumbach/electron density D-137

Appleton - Hartree's formula D-471, 717, 723, 747

Boltzmann's equation D-735

Brogli's equation/electron wave length D-688

Continuity equation D-271

Dispersion equation D-733

Distance of detection of cosmic radio signals D-192

Doppler equation D-831

Effect of magnetic field on radio signals D-687

Electrohydrodynamic drag on a wire and on a large disk

D-S55

Electron molecule collision D-249, 323

Feinstein's equation D-161

Fokker - Planck terms D-735

Hankel' s functions D-635

Huygen's principle D-161

Ionospheric absorption D-S58

Ionospheric distribution of radio waves D-264

Kramer's formula D-373, 701

Linearized fluid dynamics equation D-655

Lorentz' polarization term D-721, 723

Magneto-hydrodynamic equation D-1004

Malt - Smith's interpolation method D-733

Maxwellian distribution functions in plasma for electrons

D-656

Maxwellian distribution functions in plasma for ions D-55S

Mean electron density with height D-403

"Old" formula for rotation of plane polarization D-102

Radar equation D-293

Rice's probability distribution function D-441

Satellite radiofrequency shift D-377

Snell's law D-303, 778

Solar eclipse electron density calculation D-704

vn
Stoke' s parameters D-138

Transport equation D-99

van Vleck - Weisskopf's equation D-826

Vlasov's formula D-733

Wave-guide equations/first-order mode D-886

III. STRUCTURE AND CHARACTERISTICS OF THE EARTH'S

ATMOSPHERE

1. Atmospheric structure

Troposphere D-44, 235, 396, 530, 531, 605

Blob structure D-7

Duct mechanism D-25

Refractive index profiles D-531

Stratosphere D-375

Ozone layer D-220

Mesosphere D-243, 375, 605

Mesopause D-726

Thermosphere D-585, 605

Exosphere D-76, 169, 196, 236, 237, 242, 354, 563,

571, 573, 605, 609

Threshold of interplanetary gases D-20, 666

Electron layers D-721, 723

Ion layers D-721, 723

2. Ionospheric layers

Ionosphere D-23, 47, 571

Outer ionosphere D-14, 18, 20, 668

Layer formation D-361

D layer D-31, 41, 59, 60, 66, 127, 200, 211, 214, 223,

232, 257, 271, 435, 447, 486, 544, 545,

586, 613, 653, 703, 725, 726, 728, 741,

747, 786, 850, 875, 891, 961, 1008

E layer D-69, 77, 117, 127, 214, 233, 250, 265, 280,

339, 356, 361, 386, 423, 433, 469, 480,498,

535, 536, 540, 544, 558, 586, 613, 632, 660,

661, 670, 682, 704, 711, 720, 725, 727, 728,

730, 739, 747, 791, 802, 891, 920, 961, 973,

980, 998, 1005

Vlll
E

1 layer D-721, 722

E

2

layer D-721

Es layer D-73, 77, 193, 235, 280, 308, 441, 498, 506,

508, 537, 572, 711, 719, 724, 726, 727,

791, 838, 880, 900, 919, 966

F layer D-60, 69, 76, 99, 117, 119, 154, 176, 233, 239,

249, 265, 308, 321, 354, 378, 403, 433,

477, 489, 498, 510, 511, 558, 571, 587,

653, 654, 725, 739, 791, 851, 880, 883,

891, 920, 961, 963, 973, 994, 998, 1001,

1005

F, layer D-250, 251, 433, 535, 632, 660, 704, 711, 720,

1 721, 730, 738, 802, 888

"Valley" D-251

F9layer D-9, 49, 59, 66, 77, 189, 229, 246, 250, 251, z

295, 315, 369, 403, 425, 433, 460, 489, 506,

534, 536, 545, 603, 653, 659, 660, 661, 670,

704, 711, 717, 727-729, 802, 829, 838, 882,

888, 908, 919, 991

3. Regions and zones

Polar atmospheres D-219, 281, 589, 592, 593, 604

Auroral absorption zone: see PHYSICO -CHEMICAL

FACTORS AND PROCESSES p. xiv

Scintillation region: see- PHYSICO - CHEMICAL FACTORS

AND PROCESSES p. xiv

4. Ionospheric characteristics

Irregularities D-258, 357, 378, 416, 624, 685, 705, 731,

743, 757, 764, 854, 888, 901, 968, 1002

SID . Sudden Ionospheric Disturbances D-125, 145, 173,

213, 214, 223, 270, 271, 274, 384, 385, 450,

522, 543, 558, 591, 618, 674, 741, 889,

1005, 1008

Storms D-69, 71, 73, 99, 127, 153, 235, 285, 286, 339,

357, 522, 593, 717

Drifts D-86, 122, 280, 511, 657, 659, 829

Curves D-146

Mechanism D-154

Focusing D-598, 670, 775, 820, 869, 901, 1002

Defocusing D-820

IX
Current systems D-541, 758

Oscillations D-573

Variation D-713

Profiles D-910

See also: Radio communication disturbances, p. xxxviii

5. Atmospheric elements and factors

Thermospheric density D-585

Heavy water D-884

Clouds D-133, 229, 380, 566

Earth cloud covers D-789

Ionized clouds, Es D-411, 415, 476, 653, 919

Artificial electron clouds D-494, 501

Satellite cloud photography D-789, 1006, 1009

Temperatures D-220, 603-605, 609, 610, 756, 758, 790,

943

Stratification D-32, 33, 353

Fluctuations D-235

Satellite measurements D-550

Pressure D-33, 375, 588, 986

Winds D-235, 606, 620, 873, 966

Troposphere D-7, 371, 372

Upper air D-106, 157, 463, 510, 940

Atmosphere's "windows"

Optical window D-857, 860

Radio windows D-857, 860

U. S. " window " region maps D-887
6. Altitudes of observations

100 km

8-12

50

60

>60

<70

60-70

70

75

69-76

70-80

>85

<85

70-90

80-90

82-90

90

95

64-97

98

<100

100

km D-216

D-112, 319

D-469# 541, 844

D-668

D-586, 844, 865

D-223

D-97, 494

D-211

D-862

D-610

D-586

D-586

D-127

D-942

D-323

D-865

D-1008

D-501

D-626, 724

D-730

D- 117, 268,442,

477, 723

i>300 km

220 km D-165, 758, 915

225 D-202

225-228 ' D-943

80-250 D-940

90-250 D-519

200-250 ' D-599

300 D-980

i400 km

60-320

340

350

90-400

300-400

400

km D-747

D.548

D-548, 604, 758

D-517

D-804

D-193, 284, 297,

442, 477, 517,

558, 560, 621

*j> 200 km

^> 500 km

>100

106

111

117

60-120

70-120

120

128

100-130

130

50-150

150

80-160

161

190

<£oo

66-200

200

km D-963

D-626

D-626

D-626

D-1005

D-477

D-193

D-626

D-541

D-494

D-403

D-585

D-844

D-700

Dr 724

D-488

D-724

D-427, 604

411

420-470

475

322-483

400-500

500

km

}

D-291

D-980

D-403

D-220

D-775

D-603, 604, 740,

900

600 k,m

550 km D-985

1700 km

644 km D-291

270-650 ii D-699

650 i D-985

180-700 ii D-435

225-700 n D-943

700 ii D-247

XI
100-800

800

} 800 km

km D-986

D-548

2700

2000-3000

3000

> 3000 km

km D-886

D-17

D-620

% 900 km

885

500-900

km D-333

D-717

^ 4000 km

3555

510-3750

km D-291

D-104

> 1000 km

992 km D-293 From 5000 to 10. 000 km

1000 " D-548, 303, 604, 644-4023 km D-928,

728 6436

9654

D-291, 761

D-948

> 2000 km

From 10.000 to >1000 km D-519 36. 000 km

<fl200 D-548, 717 10, 000 km D-585, 604

1500 D-621 12, 240 D-291

1550 D-695 1000-13,000 " D-14

1700 D-767 18, 000 D-262

1936 D-291 1610-19,308 " D-551

100-2000 D-604 20, 000 D-980

1000-2000 D-598 29, 400 D-291

7. Plasmas

Plasma types

Flames D-687

Hydrogen D-263

Ion electron plasma D-354

Solar corona plasma D-590, 592

Plasma characteristics D-40, 431, 577, 615, 634, 808,

824, 914

Absorption D-687

Conductivity D-634, 687

Electron density D-615, 634, 824

Damping D-656

XII
Excitation of whistlers by sound waves D-672

Gaseous discharges D-687

Level D-137, 145

Measurements D-647

Noise generation D-700, 971

Oscillations D-905, 1004

Microwave radiation D-351, 569

Particle density D-263, 824

Particle collision frequency D-824

Radiation frequency spectrum D-688

Scale height D-393

Wave interaction D-824

Re-entry problems D-21, 224, 401, 700, 808, 824, 914

Control of radio fadeout during re-entry D-824, 825

Effects on electronic equipment D-688, 824, 825, 971

Ionization around re-entering bodies D-824, 825

Radio wave propagation in plasma D-687

Research programs D-647

Sheath properties D-700, 808, 824, 914

Shock fronts D-733

Shock layer attenuation D-224

Shock waves D-687, 763

Thermal ionization D-824

8. Characteristics of other atmospheres

Conductivity between Earth's and Sun's atmospheres D-113

Sun's atmosphere D-271, 420, 523, 675, 676, 817

Ionosphere D-292

Photosphere D-78, 113, 137, 146, 618

Chromosphere D-303, 911

Jupiter's atmosphere D-921, 931, 937, 1011

Hydrogen atmosphere D-861

See also: RADIATION p. xvii

XI 11
IV. PHYSICO - CHEMICAL FACTORS AND PROCESSES

1. Geomagnetism

Earth's magnetic field D-12, 91, 154, 173, 176, 219, 225,

264, 337, 357, 564, 584, 614, 665,

697, 721, 730, 758, 777, 845, 850,

911, 976

Electric field D-154, 157, 179

Disturbances D-123, 145, 297, 311, 618, 682, 717,

729, 757, 764, 807, 817, 912

Storms D-60, 112, 239, 262, 268, 299, 302, 346,

463, 522, 590, 592, 602, 654, 741,

764, 843, 878, 897, 948, 954, 977,

1012

Forecasting D-764, 870

SC (Sudden commencement) D-209, 253, 277,

757, 1012

Bays D-919, 963

Geomagnetic activities D-12, 50, 155, 157, 164, 177-

179, 183, 207-209, 255, 268, 281,

396, 397, 434, 452, 485, 541, 548,

582, 585, 590, 595, 662, 668, 704,

790, 959, 963, 965, 968

Miscellaneous

Sun's magnetic field D-30, 137, 163, 228, 253, 902,

911, 926, 997

SFE (crochets) D-8, 167, 173, 223, 385, 542

K indices D-154, 155, 268, 396, 463, 843, 968

Tubes of force D-354

2. Absorption D-2, 3, 5, 27, 28, 31, 48, 59, 60, 78, 104, 112,

117, 119, 134, 166, 229, 249, 253,

268, 281, 302, 312, 318, 319, 325,

338, 362, 369, 370, 391, 433, 436,

448, 454, 455, 464, 466, 469, 470,

478, 486, 542, 544, 545, 615, 616,

631, 632, 653, 654, 670, 671, 681,

682, 701, 703, 704, 719, 725, 739,

743, 762, 820-822, 851, 877, 891,

919, 964, 970, 996

Diurnal variation D-166, 822

Seasonal variation D-166

xiv
Classification

High-latitude absorption types D-990

Polar-cap absorption D-424

Negative absorption D-834

SCNA (Sudden cosmic noise absorption) D-712, 870

Miscellaneous

Absorption by water vapor D-27, 826

Absorption by oxygen D-27

Absorption by gases D-887

Absorption by clouds D-133, 229

Absorption by hydrogen clouds D-884

Absorption by collision D-712

Absorption of short waves D-820

Absorption micromeehanism D-664

Auroral absorption zone D-48, 112, 166, 230, 268, 281,

286, 414, 455, 470, 477, 486, 511,

592, 682, 683, 703, 888, 959

3. Ionization D-9, 29, 40, 60, 72, 73, 112, 117, 127, 157, 165,

176. 193, 196, 200, 214, 219, 223,

232, 249, 265, 270, 318, 332, 402,

423, 459, 464, 498, 538, 585, 586,

590, 603, 620, 668, 682, 684, 695,

704, 711, 735, 738, 741, 747, 748,

756, 777, 780, 851, 882, 920, 942,

998, 1008

Classification

Abnormal ionization D-593

Satellite-induced ionization D-414, 415, 472, 689, 833

Shock-layer ionization D-224

Shock-wave ionization D-763

UV ionization D-386, 704

Miscellaneous

Eddy formation D-157

Spiral -shaped ionization pattern D-592

Ring currents D-259

Ionization mechanisms D-410-412, 455, 488, 687,

704, 833

Sputtering D-488

Ionized oxygen layer studies D-366

Ionized clouds D-411, 415, 476

h'f (ionization profiles) D-560, 963, 996

xv
4. Scintillation D-3, 4, 6, 7, 71, 72, 74, 85-88, 106, 117, 120,

121, 154, 176, 216, 217, 230, 232,

281, 322, 372, 402, 440, 442, 460,

468, 498, 579, 740, 915, 955, 961,

964, 970, 1012

Radio star scintillation D-154, 156, 157, 165, 258, 266,

284, 298, 357, 378, 395, 396, 402,

408, 441, 463, 465, 466» 476, 477,

543, 616, 683, 702, 842, 873, 883,

900, 912, 964-966, 968, 1002, 1012

Miscellaneous

Radio star scintillation spectrum D-901

Scintillation "ridge" effect D-973

Scintillation mechanism D-156

Scintillation index D-4, 72, 155, 966

Non-ionospheric scintillation D-979

Causes of radio star scintillation D-982

5. Refraction D-3, 54, 72, 78, 89, 302, 370, 400, 443, 466,

471, 490, 530, 531, 543, 572, 598,

604, 705, 780, 823, 847, 854, 877,

881, 888, 910, 970, 1001

Wedge refraction D-774

Refraction around rockets D-721

Difraction D-297, 298

6. Reflection D-34, 77, 78, 94, 102, 150, 615, 635, 670, 704,

722, 862, 886, 888

Oblique incidence D-41, 77, 671

Reflection from sea D-1001

7. Scattering D-69, 71, 73, 74, 76, 598, 713

8. Attenuation D-34, 59, 66, 200, 224, 376, 495, 543, 566,

653, 660, 712, 739, 741, 823, 865,

889, 892, 893

By clouds D-133

See also: RADIATION p. xvii

xvi
V. RADIATION

1. Sources (See also: Other types of radiation)

a. Galaxies D-66, 93, 105, 429, 476, 629, 630, 643, 706,

709, 739, 749, 750, 751, 753, 773,

775, 783, 787, 965, 989

Milky Way D-68, 341, 342, 643, 673, 797, 857, 861,

885

Spiral structures D-93, 105, 885

Globular structures D-95

Elliptical structures D-95

b. Planets (Stars) D-284, 297, 321, 342, 408, 429, 515,

576, 663, 683, 707, 749, 750,

909, 964, 1005

Epsilon Eridani D-82, 316

Jupiter D-105, 191, 312, 408, 515, 649, 691, 718, 742,

744, 770, 772, 776, 921, 931, 937,

947, 983, 1011

Jupiter's atmosphere

Thunderstorms D-921, 931, 937, 1011

Temperature D-937

Clouds D-937

"Van Allen" Belt D-649

Mars D-515, 941

Saturn D-191, 718, 776

Tau Ceti D-82, 316

Venus D-106, 312, 408, 413, 515, 718, 937, 941

Moon D-102, 181, 247, 300, 387, 527, 749, 750, 762,

918

c. Constellations

Canis Major D-674

Cassiopeia D-3, 87, 120, 154, 155, 193, 230, 281,

357, 430, 461, 468, 511, 530, 556,

674, 677, 702, 709, 753, 773, 857,

884, 964, 968, 982

Cygnus D-117, 325, 461, 468, 511, 530, 556, 643, 674,

702, 709, 773, 857, 858, 868, 901,

966, 1002

Cygnus A D-396, 441, 677, 731, 900

Cygnus X D-967

Hydra A D-768

Jovian D-974

xvii
Perseus D-453f 674

Puppis D-674

Sagittarius D-556, 674, 885

d. Nebulas D-28, 191, 325, 476, 750, 753, 885, 979

1885 D-753

1895 D-753

M-31 D-629, 753

Type II D-988

IC 443 D-988

IC 1318 D-325

NGC 5253 D-753

NGC 7293 D-629

NGC 1275 D-453

Taurus (Crab nebula) D-138, 556, 629, 663, 702, 753,

857

Centaurus D-629

Orion D-556, 884, 1000

Spiral nebulas

Andromeda D-406, 858, 861

Elliptical nebulas D-858

e. Cosmic clouds D-885, 989

Cloud nebulas D-861

Corpuscular clouds D-364, 410, 414, 593

Dust clouds D-643

Gas clouds D-487, 644, 858

Hydrogen clouds D-861, 884

Neutral D-650

Magellanic clouds D-686, 861

f. Comets D-718, 894

The Arend-Roland comet D-894

The Burnham comet D-972

g. Radiation belts D-263, 336, 415, 479, 577

"Van Allen" belts D-414, 473, 479, 603, 654, 668, 699

Jupiter's "Van Allen Belt" D-649

Artificial radiation belts D-603

New ulterior belts D-263

Infrared bands from Earth D-376

Earth's corona D-169

xvm
h. Miscellaneous Sources

Discrete sources D-750, 753f 779, 979, 988, 989

Radio galactic systems D-884, 974

Hydrogen atmospheres D-232, 861

Extragalactic sources D-650, 753, 771, 857, 858

Extraterrestrial sources D-117, 259, 394, 429,

705, 732

HII regions D-1007

Empty sky D-145

Meteors D-32, 300, 351, 381, 613, 668, 797

Micrometeorites D-758

Near anti-galactic center D-407

Plasmas D-688

"Limit of universe" D-884

Satellite-observed high radiations D-840

i. Surveys, etc.

Radio survey of galactic plane at: 408 Mc/s D-989

85 Mc/s D-989

1390 Mc/s D-989

Southern Milky Way at 19. 7 Mc/s D-1007

Radio brightness of the sky D-405, 406

Radiation intensity D-731, 840

Variation D-731, 768

Cause D-731

Mechanism D-768, 773

Geophysical effects D-840

Metaphysical aspects D-984

2. Solar Radiation D-27, 32, 53, 61, 78, 102, 105, 146, 147,

177, 181, 200, 223, 271, 299, 301,

318, 353, 366, 371, 375, 408, 420-

422, 424, 426, 429, 434, 476, 487,

530, 597, 663, 674, 675, 706, 708,

714, 718, 749, 750, 762, 771, 790,

797, 816-818, 825, 827, 851, 868,

892, 896, 902, 923, 926, 970,

1001, 1011

xix
Variations

"Enhanced radiation, " high-intensity radio frequency spectrum D-896-899, 975,

978

Components D-630

Frequency analyses D-628

Changes due to influence of solar planets D-576

Decreased radiation D-360

3. Flares D-10, 29, 37, 41, 61, 67, 91, 101, 125, 127, 147,

149-151, 162, 163, 167, 175, 184-

187, 210, 211, 213, 214, 219, 223,

229, 232, 253, 255, 270, 271, 274,

283, 286, 299, 301, 302, 313, 318,

319, 360, 365, 383, 385, 388, 408,

410, 422, 426, 437, 450, 454, 458,

485-487, 490, 491, 541, 542, 582,

583, 586, 588, 618, 648, 652, 659,

681, 684, 699, 729, 730, 741, 749,

757, 764, 769, 798, 803, 818, 850,

862, 874, 886, 897, 902, 903, 905,

911, 926, 942, 944, 951, 978,1008

3+ flares D-283, 319, 950

H flares D-175, 184, 187, 211, 417

E limb flares D-867, 871, 902

Chromospheric flares D-905, 977

Hydrogen explosion flares D-588

4. Bursts D-167, 170, 171, 184, 186, 203, 227, 270, 271, 274,

301, 302, 346, 359, 364, 383-385,

397-399, 417, 421, 423, 428, 512,

514, 566, 597, 648, 676, 698, 770,

803, 815, 818, 830, 855, 896, 898

Burst classification D-147, 185, 512, 513, 898, 903, 975

Type I D-96, 211, 217, 254, 418, 487, 692, 803,

904 975

Type II D-5, 67, 96, 211, 245, 418, 487, 692, 803,

811 904 975

Type III D-5, 67, 96, 171, 211, 245, 254, 399, 418,

648, 690, 692, 741, 803, 905,975

Type IV D-39, 96, 277, 364, 417, 424, 487, 514, 590,

593, 627, 757, 803, 811

Type V D-905

xx
M bursts D-811

SD bursts D-811

CD bursts D-811

Chromospheric bursts D-253, 417, 418# 428, 452, 558,

627, 867

Polarized bursts D-289, 359, 810, 818

New type D-690

Burst temperatures D-421

Burst structures D-162, 975

Burst cinematograms D-902

5. Sunspots D-30, 53, 101, 148, 163, 179, 228, 230, 234, 286,

315, 331, 335, 338, 392, 538, 582,

595, 769, 796, 803, 817, 848, 859,

891, 902, 911, 926, 951, 954, 968,

998

Groups D-l

Cycles D-22, 120, 157, 308, 402, 434, -536, 820

Maximum D-402, 514, 728

Forecasting D-259, 539

Miscellaneous

Terrestrial effects D-53

Weather correlation D-23, 332, 383, 790, 948

Relation to tree rings D-332

Relation to rainfall D-332

Relation to height of lakes D-332

6. Eclipses D-l, 4, 7, 47, 65, 75, 77, 133, 150, 181, 199, 226,

234, 246, 250, 251, 257, 280, 303,

315, 366, 367, 429, 433, 435, 482,

489, 535, 548, 632, 660, 661, 671,

704, 708, 711, 729, 738, 749, 756,

765, 782, 786, 791, 802, 820, 829,

863, 873, 882, 997

7. Solar structure D-718, 989

Sun's atmosphere D-271, 420, 523, 675, 676, 817

Motion D-674

Chromosphere D-303, 911

Photosphere D-78, 113, 137, 146, 618

Ionosphere D-292

xxi
X-ray region D-270

Sun's gravitational field D-982

Sunspot regions D-135

Sun's radio picture D-124, 708

Sun's radio spectrum D-513, 628, 997

Solar disk D-289, 597, 738, 779

Solar corona D-249, 298, 303, 490, 701, 708, 744, 882,

905, 1004, 1008, 1013

8. Solar activities, etc. D-50, 119, 143, 236, 269, 313, 315,

321, 328, 383, 412, 423, 429, 518,

536, 537, 579, 583, 588, 604, 614,

646, 659, 668, 702, 719, 720, 817,

859, 919, 924, 944, 948, 998,1010

Quiet sun D-146, 148, 218, 255, 303, 361, 530, 707, 708,

750, 997

Quiet areas D-135

Disturbed sun D-218, 255, 361, 698, 750

Active areas D-4, 148, 177, 178, 228

Storms and disturbances D-64, 123, 163, 189, 220,

228, 255, 271, 579, 627, 698, 729,

848, 977

Bubbles D-926

M-storms D-729

Coronal irregularities D-633, 690

Streamers D-579, 590, 593, 745, 905, 919, 954

Indices D-80, 422, 537, 538, 606

Winds D-479

Temperatures D-893, 970

Rises D-113

Brightness temperature D-135

Burst temperature D-421

Coronal temperature D-303, 663, 708, 734

9. Solar - Terrestrial relationships D-l, 22, 37, 179, 184, 212,

215, 218, 254, 286, 314, 375,

383, 614

10. Lunar radiations D-102, 181, 247, 300, 387, 527, 749, 750,

762, 918, 936

XXI
Surface reflectivity D-161, 326, 351, 379, 380, 445, 607,

622, 736, 737, 832, 913, 976, 994

Using light waves (spark discharge) D-607

Rough effective D-293

Quasi-smooth D-293, 736

Radio mapping D-622

Radar cross section D-913, 976

Radar "illuminated" area D-607

Conductivity of lunar rocks D-918

Surface composition D-247, 913

Surface topography D-913, 976

Surface layer D-222

Miscellaneous

Lunar variations D-506

Lunar physical conditions D-1010

Lunar electric currents D-508

Lunar oscillations D-544

Lunar magnetic field D-936

Lunar tracking D-710, 994

Lunar rocket impact observations D-933

11. Other types of radiation

Cosmic radiation D-39, 105, 151, 163, 164, 200, 218, 220,

223, 229, 346, 349, 350, 364, 426,

450, 452, 481, 509, 522, 548, 550,

558, 572, 577, 586, 590, 604, 643,

673, 674, 681, 695, 699, 710, 750,

751, 756, 758, 759, 767, 830, 845,

903, 911, 923, 926, 936, 942, 951,

976

Soft D-112

Hard D-621

Cosmic-ray electrons D-253, 260, 350

Bursts D-350

Energy spectrum D-260

Particle radiation

Betatron D-618

Cyclotron D-260, 563, 564, 569, 834

Cerenkov D-834

C02 D-550

Electron D-569

Secondary D-519

xxm
Galactic deuterium D-787

Nitrogen molecules D-585, 586, 604

Oxygen molecules D-585, 586, 604

Miscellaneous radiations, etc.

Background radiation D-394

Black body radiation D-392, 515

Bremsstrahlung D-219, 270, 618, 688

Serenkov radiation D-189, 242, 349, 834

Gamma rays D-473, 618

H Ob D-175, 184, 214, 397, 398

Hx D-18

Incident D-220, 284

L CO D-112, 125, 126, 214, 232, 397, 509, 586, 686, 874

Light intensity

Red D-756

Yellow D-756

UV D-61, 112, 129, 214, 220, 223, 486, 492,

536, 588, 602, 704, 730, 756,

758, 767, 845, 926, 927

X-ray D-61, 112, 126, 127, 214, 232, 397, 536,

586, 758, 767, 845, 874

Flares D-127

Flux D-26, 988

3A-X D-874

Nonthermal D-61, 189, 382, 613, 885, 988, 989

Galactic D-987

Polarized D-138

Radiation spectra D-335, 629

Mechanism D-271

Intensity D-284, 416, 549, 753

Reflected D-220

Thermal D-134, 247, 382, 712, 885, 989

Ionospheric D-610

Galactic D-987

VI. PARTICLES

Electron characteristics

General D-354, 1003, 1008

Artificial electron clouds D-494

Cosmic ray electrons D-260, 350

xxiv
Cosmic ray electrons, bursts D-350

Cosmic ray electrons, energy spectrum D-260

Electron "blobs" D-976

Electron production D-219, 1005

Electron temperatures D-259, 403, 448, 571, 610,

656, 747

Super-thermal electrons D-270

High-energy electrons D-834

Electron collision frequency D-19, 569, 682, 685, 721,

723, 725, 728, 735, 739, 747,

891, 961

Electron collision frequency in plasma D-824

Electron/neutral particle collision frequency D-615

Electron/molecule collisions D-249, 323, 569, 615, 664

Electron/Electron impact D-249

Free-free transitions D-189, 701, 834

Scattering by free electrons D-129, 259, 625, 664,

687, 725, 728, 1008

Free electron motion in pure nitrogen D-323

Electron velocity D-195, 263, 404, 627, 747, 895

Non-thermal motion D-630, 834, 688

Ionospheric vertical transport mechanism D-829

Relativistic electrons D-809, 834, 905, 988

Relativistic solar particles D-61, 593, 711

Electron density

General D-17, 18, 113, 200, 233, 239, 259, 263, 266, 337,

400, 415, 448, 471, 503, 572, 587,

665, 682, 685, 721

Distribution with height D-14, 129, 236, 793

Distribution with satellite height D-920

In ionosphere D-19, 49, 63, 158, 159, 239, 259, 264, 265,

271, 289, 297, 298, 306, 361, 369,

393, 401, 443, 477, 534, 536, 541,

555, 565, 571, 604, 605, 620, 624,

626, 635, 654, 665, 696, 697, 717,

725-727, 774, 778, 838, 874, 875,

891, 908, 923, 943, 961, 980, 985,

971, 994, 996, 1008

Above the known atmosphere D-196, 262, 571, 777, 961,

976, 991, 996

In the vicinity of a satellite D-262, 991

Between observer and satellites D-991

In exosphere D-196, 589, 604

In plasma D-615, 634, 824

In interplanetary space D-113, 255, 259, 289, 354, 605

xxv
Between Earth and other planets D-976

Cislunar D-976

In solar corona D-303, 686, 690, 708

Per cm

2 D-297, 396, 962

Per m

2 D-717

Per cm

3

D-20, 102, 204, 237, 262, 403, 585, 589, 604,

626, 723, 724, 728, 777

Per cubic inch D-113

Other particles

Calcium, ionized D-104

Charged particles D-119, 366, 534, 585, 699, 845

Clouds D-12, 380

Layers D-366

Deuterium D-787

Collision frequency of gas particles D-748

Electronic conductivity of ionized gas D-735

Energetic particle flux D-253, 286, 323, 684

Gas mist shells D-868

Interplanetary gases D-976

Relativistic gas dynamics D-686

Helium D-603

Hydrogen D-650, 701, 779, 787, 792, 795, 868, 926

Hydrogen atoms D-184, 252, 432, 604, 605, 982

Hydrogen, neutral D-136, 354, 556, 604

Hydrogen collision D-1000

Hydrogen ions D-354, 792

Geomagnetic storm particles D-897, 903, 977

Spiral pattern D-301

Ions D-76, 112, 200, 354, 488, 571, 654, 985, 1008

Ion belts D-98

Ion beams D-318

Ion density D-263, 318, 590, 618, 634, 721, 723,

730, 792

Ion Stormer orbits D-318, 590, 618

Ion temperature D-656

Interstellar particles D-982

Movement by solar attraction D-705

xxvi
Mass spectrometry up to 900 km D-985

Meteoric dust D-376, 604

Molecules

Molecular diffusion D-71

Elastic collision of air molecules with satellites

D-600, 833

Photoionization D-94

Neutron intensity D-549

Neutral particles D-354

Nitrogen D-585, 586, 604, 985

Nitric oxide D-112, 501, 586

Nuclei

High energy positive nuclei D-164

Nucleon intensity D-151

Galactic nuclei D-405

Oxygen D-459, 585, 586, 604, 684

Atomic oxygen D-985

Ions D-94, 354

Particle collision

Coulomb type D-735

Atomic impacts D-488

Bombardment from stars D-342

Particle diffusion D-809

Particle flux D-386

Particle"Van AllenM flux D-253

Photons D-99

Protons

Auroral protons D-142

High energy protons D-590, 990

Solar protons D-112, 113, 319, 424, 481, 563, 604,

628, 684, 695, 795, 830

Solar particles D-977, 990, 1011

Corpuscular interaction/ atoms D-592, 684, 752, 764

Corpuscular streamers D-404

Flare particles D-219, 286, 318, 319, 592, 621

XXVll
VII. WAVE CHARACTERISTICS

1. Frequencies and wave bands

Cps. D-878

10 -45 ii D-268

50 D-473

750 ii D-268

ELF (C3 Kc/s. 1000 - 100 km TO D-573, 792, 878, 879

<1 Kc/s D-339

VLF ( <30 Kc/s. 100 - 10 km 71) D-5, 189, 206, 237, 242,

385, 483, 564, 573, 591, 636, 638,

865, 866

10 cps - 10 Kc/s D-268

4 - 12 ii D-75

<15 D-94, 97, 101, 140, 199, 209, 775

15 D-879

16 D-741, 862

19.6 • D-862

10 - 20 D-886

27 ii D-75, 211, 447

1 - 30 D-237, 245, 865

Kilometer wavelengths

11 km D-164, 418

21 km D-716

Diurnal phase shift data D-886

LF ( <300 Kc/s. 10 - 1 kmA.) D-97, 100, 199, 204, 206,

208, 268, 1004

Miscellaneous

2 - 40 Kc/s D-206

51.95 D-862

8 - 69 D-435

8 - 70 D-786

100 D-486

150 D-459

MF ( <3 Mc/s. 1000 - 100 m A) D-610, 678, 680

<1 Mc/s D-171, 202, 204, 216, 246, 517, 678, 680,

775, 776

>1 Mc/s D-166, 170, 280, 558, 671, 678, 690, 786

XXVI11
HF ( 3 - 30 Mc/s. 100 - 10 mA,) D-112, 139, 143, 153,

172, 173, 237, 245, 286, 376,

378, 412, 821

3 - 10 Mc/s

10 - 20 Mc/s

D-77, 171, 558, 626, 660, 661, 690, 721,

723, 765, 775, 885, 891, 971, 1005

D-67, 78, 96, 100, 101, 128, 131, 170,

171, 190, 233, 245, 306, 308, 375,

443, 447, 471, 475, 478, 489, 545,

555, 561, 568, 598, 601-604, 644,

660, 665, 697, 739-742, 776, 828,

855, 870, 876, 877, 936, 978,

1005, 1007

20 - 30 Mc/s D-6, 9, 35, 43, 48, 49, 66, 68, 75, 81,

96, 100, 101, 121, 217, 255, 279,

379, 388-390, 425, 430, 469, 472,

562, 645, 652-654, 682, 684, 712,

776, 781, 783, 864, 931, 964, 967,

996, 1005

Miscellaneous

4 - 14 Mc/s D-170

<15 i D-352

2 - 15 D-835

1 - 16 D-558

5 - 30 i D-765

HF meter wavelengths (see also: Miscellaneous meter

wavelengths)

10

11

14

14.6

16.7

20

21

32.2

m D-416

D-408, 413

D-380

D-339, 343

D-343

D-246

D-124

D-343

VHF (30 - 300 Mc/s. 10-lmX) D-73, 143, 235, 241,

30 - 40 Mc/s

40 - 50 Mc/s

262, 286, 465, 466, 530, 531, 653,

682, 873, 881, 990, 1013

D-16, 67, 81, 101, 149, 165, 281,306,

357, 378, 436, 536, 555, 561, 603,

604, 613, 644, 653, 665, 697, 780,

783, 787, 828, 968, 977, 1013

D-9, 8, 43, 117, 142, 284, 390, 436,

568, 645, 653, 732, 901, 982

XXIX
50 - 60 Mc/s D-67, 230, 440, 441, 684, 1001

60 - 70 " D-464

70 - 80 " D-101, 118-120, 313, 510, 555

80 - 90 " D-30, 989

90 - 100 " D-117, 165, 677, 739

100 - 200 " D-25, 37, 49, 64, 67, 93, 101, 142,

177, 185, 187, 196, 197, 201-203,

226, 227, 255, 397, 436, 440, 441,

452, 490, 514, 544, 565, 579, 597,

633, 643, 674, 679, 698, 714, 818,

824, 832, 902, 928, 962, 1001

D-5, 7, 25, 141, 171, 201, 394, 407,

436, 468, 731, 732

200 - 300 Mc/s

Miscellaneous

<30

40 - 70

105 - 140

30 - 180

40 - 180

215 - 190

40 - 240

<250

23 - 265

Mc/s D-945

D-901, 904, 905

D-254

D-390

D-244

D-975

D-903

D-512

D-245

VHF meter wavelengths D-15, 53, 96, 217, 228, 259, 298,

300, 303, 421, 423, 424, 627, 690,

708, 811, 871, 897

1.5

1.18

3.7

4

4.1

4 - 6

6.7

1.4 - 1.788

m D-184, 924

D-228

D-511, 773

D-301

D-223, 302

D-150, 299

D-773

D-297

D-65

UHF (300 - 3000 Mc/s 10 - 1 dm A ) D-231, 262, 326,

395, 396, 465, 466, 530, 531, 844

300 - 400 Mc/s D-171, 326, 732, 994

400 - 500 " D-5, 67, 226, 231, 326, 405,

440, 468, 514, 679, 989,

1003

500 - 600 " D-15, 255, 859

700 - 800 " D-426

800 - 900 " D-116, 679, 649

XXX
900 - 1000 M c/s D-26, 191

1000 - 1500 i D-4, 7, 192,

629, 1390

359, 618, 625,

2000 - 2500 i D-336, 359, 538

2500 - 3000 i D-67, 145, 149, 186, 187, 226,

629, 859, 913

Miscellaneous

70 - 130 Mc/s D-896-899

26 - 408 • D-121

51 - 408 D-676

25 - 580 D-830

90 - 580 D-256

100 - 580 " D-512, 513, 803

100 - 600 D-514

64 - 910 1 D-394

18. 3 - 1200 I D-629

19. 7 - 1390 I D-987

The 1420 Mc/s line (See also the 21-cm line below)

D-136, 192, 252, 316, 417, 527

30 - 3000 Mc/s D-832

Decimeter wavelengths D-217, 417, 422, 423, 429, 627,

871, 974, 1011

1 dm (10 cm. The S-band) D-146, 148, 224, 649,

700, 913

1.3 " (10.3 cm ) D-719

1. 7 " (10. 7 cm ) D-50, 147, 186, 422, 518, 537,

859

2 " (20 cm ) D-646

2. 1 " (21 cm The neutral hydrogen line) D-136, 192,

431, 432, 556, 650, 750, 751,

797, 861, 884, 885

2.3 " (23 cm The L -band) D-700

3. 1 " (31 cm ) D-691

5 " (50 cm ) D-859

5. 5 " (55 cm ) D-428

SHF (3000 - 30. 000 Mc/s. 10 - 1 cm A)

3000 - 4000

4700

8000

9000

22, 000

10, 000

Mc/s D-4, 5, 7, 167, 359, 445, 679,

812-816

" (C-band) D-970

D-191, 932

D-27, 65, 226, 359, 370,566,

618, 815, 816, 824, 873

D-974

XXXI
Miscellaneous

62 - 9, 400 Mc/s D-123

67 - 9500 D-811

12. 5 - 10f 000 D-967

60 - 10, 000 D-167

250 - 10, 000 D-910

1000 - 10, 000 D-192, 945

300 - 11, 000 D-307

600 - 24, 000 D-628

18, 000 - 35, 000 D-15

Centimeter wavelengths D-53. 270. 300. 303. 420. 42]

423, 424, 515, 627

1. 25 cm D-181

1.63 D-918

1.9 D-484, 710

3 ' (X-band) D-248, 700, 736, 800, 941

3.15 D-138, 515, 718

3.2 D-6, 65, 271, 371, 372, 420, 423

3.4 D-719

6.38 ' (C-band) D-700, 970

8.3 i D-1000

9.4 D-515

9.6 D-988

EHF ( >30. 000 Mc/s, K 10 mm A.)

Millimeter wavelengths D-478, 827

1 mm D-826

1.5 i D-762

4

•I D-387

4.3 ii D-134, 135

7 - 8

I D-892, 893

8.5 ii D-274

8.6 i D-133

8.7 D-3, 484, 495, 710

Other frequencies

24 KM c/s D-247

35 D-247

XXXI
Miscellaneous bands, etc.

X - band D-248, 700

C - band D-700, 970

S - band D-224, 700

L - band D-700

The 21-cm line of neutral hydrogen D-136, 192, 252,

316, 417, 431, 432, 527, 556,

650, 750, 751, 797, 861, 884

885

Wide band D-788

Radio window ( \ 1 cm - 20 m) D-857, 860

Optical window (3000 - 30,000 A) D-857, 860

MUF (Maximum usable frequency) D-308, 434, 746

LUF (Lowest usable frequency) D-746

Wave types

Extraterrestrial radio waves D-54, 128-130, 136, 287, 297,

298, 335, 340-342, 344, 345,

392, 395, 400, 416, 442, 460-

462, 464, 469, 474, 543, 964

Gamma rays D-310, 473, 618

Hydrogen waves D-885, 1000

Light waves

Asteroidal light curves D-688

Infrared D-925

Spark discharges D-607

Long waves D-771, 786, 798, 862

Plasma waves D-189, 288

Longitudinal D-19

Shock waves D-189, 523, 733, 1000

Short waves D-888, 924

Sound waves D-672

Thermonuclear D-585, 603, 672

Argus experiment D-603

Wave characteristics

Fading D-43, 70, 123, 231, 246, 257, 258, 425, 548, 597,

603, 756, 842, 843, 910

Blackouts D-6, 311, 455,595, 867

Re-entry predictions D-700, 825

Auroral -zone blackouts D-166, 590, 592, 593

Distribution by G. M.T. D-311

Distribution by Russian isochrons D-311

xxxiii
"Dropouts" D-6, 415, 473, 895

Fadeim D-308

Fadeouts D-125, 163, 167, 172, 173, 213, 232,283,

299, 308, 415, 454, 485, 491,

652, 729, 764, 919, 920, 942,

951

Statistics D-796

Long- duration fades D-964

Polar_cap blackouts D-166, 277, 464, 470, 590, 592,

593. 684. 725, 728

GSWF (Gradual short-wave fadeouts) D-8

SWF (Short-wave fadeouts) D-175, 870, 871

SSWF (Slow short-wave fadeouts) D-8

SSWF (Sudden short-wave fadeouts) D-8

Miscellaneous

Wave interaction D-323, 807

Wave polarization D-137, 138, 196, 228, 264, 399,

443, 471, 530, 649

Mechanical energy conversion into radiofrequency

emission D-523

Re-entry fading D-825

Transversal mechanism D-672

ECHOES

Echo types

From: Auroras D-117, 465, 466, 477, 1012

Jupiter D-259, 408

Mars D-259

Mercury D-259

Meteors D-73, 281, 465, 466, 476, 477

Moon D-20, 26, 49, 128, 158, 161, 180,

196, 231, 293, 326, 379, 380,

381, 465, 466, 477, 565, 619,

622, 832, 913, 916, 961, 962,

976 994

Sun D-139, 259, 381, 408, 690

Sun delayed radar echoes D-139

Sun corpuscular clouds D-410

Venus D-259, 408

Miscellaneous

Delayed echoes D-98, 139

"Ghost" signals D-948

Spread-F echoes D-73, 74, 87, 88, 120, 155, 156,

176, 258, 378, 402, 441, 498,

572, 653, 724, 726, 727, 880,

900, 912, 915, 963, 965

xxxiv
Quiet echoes D-73

Echo enhancement D-411, 414

Echo intensity D-379

Echo mechanism D-408

Influences

Doppler effects D-9, 21, 33f 35, 42, 89, 109, 130,

259, 267, 292, 304-306, 322, 373,

377, 412, 431, 432, 443, 497, 530,

553, 562, 598, 620, 622, 644, 645,

665, 697, 828, 831, 847, 856, 961,

976

Faraday effects D-6, 9, 49, 63, 137, 138, 158-160,

165, 264, 289, 305, 309, 348, 377,

393, 466. 471, 503, 565, 587, 598,

604, 697, 780, 847, 856, 961, 962,

994

Satellite signals D-81, 159, 160, 165, 378, 560,

717, 780

Cotton mouton effect D-598

Propagation modes

Double-hop D-246

Long distance HF D-589

Magneto-ionic D-12

Scatter D-34, 889

Mechanisms D-73, 259

Sputtering D-488

Free electrons D-259

Backscatter D-176, 489

Ionospheric scattering

F-scatter D-60, 883

O-mode D-880

Turbulent irregularities D-889

Statistical behavior D-889

Z-mode D-880

Single-hop D-246

Whistler mode D-794

Y-mode D-680

Propagation media

Electron plasma D-354, 373

Interstellar gases D-979

Plasma D-224, 373, 615, 634, 824, 825

XXXV
Spherical ionized shell D-129

Solar ionosphere D-292

Unionized medium D-129

Very high altitudes D-920, 923

Propagation characteristics, etc.

Anomalous propagation D-309

Basic physics of propagation D-749

Vertical propagation tests D-337

Wind-tunnel propagation tests D-700

Propagation measurements D-721

Radio ducting D-910

Rocket experiments D-624, 626, 721

VIII. RADIO COMMUNICATION

Experimental transmissions D-109, 138, 189, 238, 240, 442,

461, 480, 489, 543, 607, 680, 694,

700, 721, 722, 781, 788, 794, 832,

945, 981, 994

Control experiments D-153, 343, 472, 772, 781

Dipole belts D-932

Gamma rays D-310

Hydrogen line D-82, 90, 116, 136, 192, 252, 316

Light waves D-607, 925

Meteors D-38

Moon relay D-736, 962

Satellite relay D-57, 109, 307, 781, 788, 852

Telephone D-307

TV D-124, 291, 536, 789, 853

See also: Propagation characteristics

Space exploration D-92, 259, 275, 292, 310, 351, 419, 479,

503, 529, 572, 577, 585, 600-604,

616, 620, 665, 755, 763, 771, 789,

806, 831, 847, 849. 856, 890, 906,

907, 909, 916, 920, 933, 934, 944,

948, 971, 981, 999

Earth-Moon distance measurement D-913

Lunar probes D-62, 90, 222, 326, 379, 622, 916, 933,

934, 936, 961, 962, 994

Re-entry problems D-700, 824, 825

Antenna efficiency D-493

Plasma wakes D-655, 656

Radar signals D-373

See also: Fading, p. xxxiii

xxxvi
Communication links and paths

Dark hemisphere D-164, 200, 318, 336, 486, 770

Sunlit hemisphere D-119, 172, 318, 336

Rocket - ground D-265, 337, 480, 517, 571, 587, 721,

722, 723, 999

Satellite - ground D-6, 9, 20, 24, 25, 42, 43, 63, 81,

89, 130, 159, 160, 198, 261, 262,

279, 304, 306, 322, 348, 369, 376-

378, 389, 390, 411, 412, 415, 425,

509, 553, 555, 560-562, 571, 598,

599, 600, 603, 619, 620, 646, 689,

696, 755, 794, 804, 805, 838, 840,

847, 864, 895, 906, 908, 909, 915,

916, 945, 971, 999

Space - Earth D-310, 852, 856

Mars, Venus, Moon - Earth D-856

Space — space D-310, 856

Path lengths

6000 Km D-598

7000 D-589

7040 D-772

8000 D-469

10, 000 D-369

15, 000 D-888

16,000 D-369

Field strength D-109, 367, 369, 660, 661, 671, 703,

719, 862, 971

Forecasting D-9, 172, 178, 295, 308, 331, 338, 538,

693, 746, 764, 870

Accuracy D-434, 576

Diurnal phase shift D-886

Systems D-572, 852, 856

FM - PM D-853

Future trends D-925

Problems of international nature D-6, 173, 174, 208,

241, 276, 481, 814, 852

Global radio communication

Moon relay D-736, 962

Satellite relay D-57, 109, 307, 781, 788, 852

Telephone D-307

TV D-124, 291, 536, 789, 853

xxxvii
Transoceanic and transcontinental

non-interference

Communication D-945

International Bodies

I G Y World Data Center D-328

Internat. Astron. Federation D-952

Council of Scientific Unions, Mixed Commission

on the Ionosphere D-946

Internat. Radio Consultative Committee, Study Group IV

D-945

Internat. Telecommunication Union D-945

URSI, Worldwide Network on Solar Radio Emission

D-814

World Warning Agencies D-241

Radio navigation

Lunar tracking D-484, 551, 710

Radio star tracking D-484

Solar tracking D-484

Interplanetary tracking D-529

Radio communication disturbances

Radio wave propagation disturbance index D-843

Es D-73, 77, 193, 235, 280, 308, 441, 498, 506, 508,

537, 572, 711, 719, 724, 726, 727,

791, 838, 880, 900, 919, 966

Focusing p. ix

P. S.C. (Polar sudden commencement) D-386

"Rise and set" effects D-18, 77, 94, 851

Satellite rotation D-165

Scintillation p. xvi

Solar activities p. xxii

SC (Sudden commencement) D-209, 253, 277, 751,

1012

SID (Mogel-Dellinger effects) D-125, 145, 173, 213,

214, 223, 227, 270, 271, 274, 384,

385, 450, 522, 543, 558, 591, 618,

674, 741, 867, 889, 1005, 1008

World-wide disturbances D-165, 450, 590

See also: Ionospheric characteristics, p. ix

and Geomagnetism p. xiv

XXXV111
Miscellaneous

foF2 (Critical frequency F2) D-315, 379, 393, 534,

537, 538, 568, 654, 661, 662,

678, 743

h'f (Virtual height) D-433, 671, 738

Noise, sferics (atmospherics) D-47, 62, 241, 351, 435.

Radio noise spectrum D-524

Cosmic noise D-10, 48, 59, 62, 110, 143, 205, 206,

229, 424, 429, 447, 545, 652-654,

678, 680, 682, 740, 741, 743, 783,

835, 874, 954, 966, 971, 990, 996

SCNA (Sudden cosmic noise absorption) D-712, 870

Extraterrestrial origin D-44, 236, 300, 312, 340,

343, 461, 739, 742, 771

Solar noise D-5, 15, 29, 47, 50, 141, 143, 149, 170,

201, 217, 224, 226, 285, 299, 300,

331, 339, 340, 347, 516, 523, 579,

582, 606, 630, 673-677, 733, 734,

770, 812-814, 843, 859, 870, 871,

902, 911, 977

Dawn chorus D-ll, 12, 183, 237, 483, 563, 613,

636, 637, 878, 954

Mechanism D-564

LF D-189, 268

Pips D-676

Noise

From all over the sky D-613

Peculiarities D-118, 119, 638

Polarization D-810

Circular D-30

Storms D-171, 185, 189, 202, 490, 514, 810

Tropospheric noise D-610

Sferics (atmospherics) D-44, 75, 96, 119, 151, 199,

200, 312, 339, 383, 385, 418, 572,

591, 707, 716, 765, 791, 878

Early experiments D-339-343

Grinders D-211, 398, 485, 591, 798, 950

Hiss D-237, 268

Audio-frequency hiss D-878, 879

XXXIX
Sweepers D-245

Whistlers D-ll-14, 104, 140, 152, 169, 183, 190,

236, 263, 334, 354, 381, 554, 585,

609, 636-638, 672, 728, 878, 954,

959

Trains and pairs D-334

Long and short D-334

Nose whistlers D-777

Components D-778

Dispersion curves D-793, 795

Frequency and time relationship D-792

Propagation in ducts D-778

Reception

Diurnal variation D-959

Trapping D-778

IX. METHODS AND TECHNIQUES OF OBSERVATION

Absorption

To determine absorption in the path of radio sources D-325

To measure absorption of short waves in the ionosphere

D-820, 877

To plot absorbing parts of the auroral zone D-888

Amplitude, synchronous measurement D-473

Analysis of data D-59, 723

Of Faraday fading D-S91

Of radio and magnetic data D-542

Matrix method D-587

Attenuation measurement methods D-134, 135

Balloon methods D-32, 618, 696

Computer programming for determination of satellite orbits D-282

Technique for analysis of radio and optical data/satellites

D-526

Density determination of upper air D-847

Direction finding measurements D-130, 322

Dispersion

Ionosphere D-587

Whistlers D-140, 793

Doppler methods D-19, 322

Shifts/simultaneous measurements D-306, 389

Measurements/satellites D-828

XL
Electrons

Collision frequency D-917

Concentration with height D-14

Content of the ionosphere D-32, 240, 697, 721, 722

Content of the upper ionosphere D-305, 306

Content below satellite height D-443, 471

Density profiles D-86

Density in the solar corona D-686

Langmuir's method/electrons, ions D-844

Local density from a satellite D-794

Radar method to detect cislunar electron density D-976

Six techniques of measuring total electron density D-976

Faraday fading. Method of analysis D-991

Focusing of radio waves in the ionosphere. Method of computation D-869

Harmonic frequency system. Method of measurement D-722

ICBMtests D-224

IRBMtests D-224

Interferometer techniques D-555

"Minitrack" D-619

Sea interferometer D-966

Ionization

Ionized oxygen layer. Method of study D-366

Ionization density D-917

Ionization density. Method of U. S. Naval Research Laboratory

D-844

Ionospheric irregularities D-624

Roughness index. Method of estimation D-888

Measurements

Matrix method/ analysis D-587

Microwave techniques D-243

Millstone Hill back scatter measurements/infrared D-1003

G.M.Minnis' method D-738

Simultaneous measurements D-6, 7, 13, 121, 152, 160,

441, 963, 974

Continuous measurements of ionospheric deviation of

signals from discrete sources D-440

Lunar measurements

Fading rate of moon echoes/prediction D-231

Mapping method/ radars D-622

Probes D-62

Size and speed of motion of lunar patches. D-197

XLI
Nebulas

Kinetic temperature of gas nebulas/ determination D-1000

Noise

Cosmic noise/ automatic recording D-430

Cosmic noise ^ 1 Mc/s. Method of recording D-678

Cosmic noise techniques D-470, 990

Cosmic noise/Total attenuation measurements D-545

Extraterrestrial noise/ continuous monitoring D-206

Optical methods

Optical radar methods D-235, 290, 992

Plasmas

Plasma properties/ hypersonic projectiles D-647

Plasma sheath properties/Experimental methods- D-700

Plotting methods

Absorbing parts of auroral zone D-888

Semilog plotting of the volt-ampere characteristics of a probe

D-448

Polarization measurements D-138, 399

Radar methods D-51, 165, 503, 685, 1007, 1013

Cislunar electron density D-976

Lunar mapping D-622

Radar space observatories D-222

Radiation

Intensity measurement, using a single Geiger-Muller tube

D-840

Intensity variation of ionizing radiation D-271

Trapped radiation. Method of calculation D-205

Radio methods D-32, 51, 349, 500, 674

CW reflection techniques D-399, 830

Oblique measurement techniques D-409

Ionospheric drifts D-657

Cross-correlation detection technique/ air space navigation

D-993

Cross modulation D-685

Elimination of ionospheric refraction effects from high altitude

transmitters D-89

Faraday fading/satellites D-717

High-frequency radio techniques D-349

Monte Carlo technique D-296

Optimum radio operation time D-746

Phase-sweep techniques D-683

XLII
Pulse amplitude techniques D-455

Pulse echo method/time measurement D-607

Radio paths in ionosphere D-18

Riometer methods D-699

"Rise and set" methods D-19

Rocket and satellite observations D-533

Spaced-receiver techniques D-197, 461, 463, 659, 772, 773

Triangulation D-118, 122, 372, 511, 824, 657, 901

Swept-frequency techniques D-399, 830

Radio-astronomy methods

Experimental methods D-706, 854

Studying ionosphere, using extraterrestrial radio waves D-543

Techniques and methods/ review D-557

Rocket methods D-21, 32, 353, 500, 504, 517, 587, 639, 721,

723-725, 727, 728, 747, 754, 758,

874, 933, 934, 936, 944, 986

Satellite methods D-51, 56, 57, 240, 241, 501, 504, 525, 584,

639-641, 654, 699, 727, 754, 760,

737, 775, 788, 789, 794, 799, 828,

845, 847, 849, 887, 927-929, 932,

939, 961, 981, 985, 986, 991,

1006, 1009

Cloud photography (TV) D-1009

Controlled interspaced satellites/ piloting system D-551

Control system method/ orbiting astrophysical laboratories

D-909

Determining electromagnetic properties of interplanetary gases

D-21

Orbits of satellites from radio data D-282

Orbits of satellites from noisy radar data D-999

Orbits of satellites from their radio signals D-198,

267, 282

Position of orbiting satellites D-89, 625

Enabling observations from satellites at <^15 Mc/s D-352

Marine navigation D-439

Reconnaissance D-363, 478, 503, 552, 640, 841, 799

Smoothing satellite data D-805

Stabilizing satellites for directed radio power D-307

Tracking methods D-525, 553, 617

Ship observations D-749

XLIII
Sounding

Cosmic ray sounding D-943

Echo sounding D-558, 994

Ionospheric sounding D-440, 652, 829

Vertical D-284

Space

Method of checking coherency of radio "space signals" D-252

Method of detecting outer atmospheric ionized hydrogen D-792

Spectrometry measurements D-985

Spectroscopic methods D-243

Statistical methods D-266, 296, 365, 532

Stars

Radio star scintillation techniques D-122, 216

Starlight intensity effects. Method of computation D-842

Sun

Overcoming eclipse effects on radio waves D-632

Solar radiation measurements D-134, 135

Surveying distribution of radio emission over the disk D-124

Survey and Reviews

Of direct and indirect methods of observations D-844

Of methods and techniques D-494

Of radio astronomical techniques D-750

Of U. S. A. and U. S. S. R. 's satellites and methods of observation D-847

Theoretical methods D-738, 746, 792, 793, 805, 991

Ultrasonic methods D-992

Upper air density D-847

Velocities in the ionosphere D-86

Visual methods of observing rockets and satellites D-532

Danjon's visual method D-216

Whistlers

Chance coincidence of whistlers. Method of computation

D-152

Dispersion D-140, 793

X. INSTRUMENTS AND EQUIPMENT

Antennas (See also: Telescopes ) D-26, 104, 189, 272, 347,

396, 517, 603, 896, 944, 1013

Circularly polarized antennas D-876

Coupling effects D-914

Horn antennas D-518

XLIV

.
Automatic

Data-processing systems D-683

Frequency-shift counting D-35

Ionosondes D-283, 441

Multi-frequency equipment D-704

Tracking filters D-24

Cerenkov detectors D-426

Computers

EDSAC D-296

IBM - 704 D-1008

Siliac computers D-562

Corpuscular stream indicators D-404

Counters . Gas counters D-349

Geiger counters D-253, 415, 549, 618, 621, 710

Halogen counters D-427

Photon counters D-874

Scintillation counters D-349

Statistical counters D-719

Direction-finding systems D-77, 208

DOVAP (Doppler velocity and position) systems D-528

Electron multipliers D-216

Golay detectors D-762

Integrating ionization chambers D-618

Interferometers D-124, 146, 228, 229, 254, 265, 402, 403, 420,

421, 423, 442, 468, 553, 566,

579, 597, 649, 683, 708, 801,

813, 815, 894, 904, 964

Christiansen's interferometer D-417

Dispersion interferometer D-980

Ion traps D-263

Kolhorster cosmic-ray apparatus D-163

L-band beacons D-969

Navigation

All-weather radio sextants D-484, 496

"Astro" celestial navigation systems D-438

Celestial navigation systems D-551

Combined radio telescope - radio sextant D-495

Radio sextants D-710

U. S. Navy radio sextant AN/SRN-4 D-551

Optical masers D-925

Oscilloscopes D-256

Triple-beam oscilloscopes D-659 .

XLV
Panoramic ionosphere recorders D-738

Stations D-265

Pfund sky compass D-710

Photocells D-607

Photo detectors D-799

Multipliers D-349

Photon counters D-874

Proton precision magnetometers D-104

Radars D-607, 910, 1013

Equipment D-299

Gordon's 400 Mc/s space radar D-140

HF radars D-153

Millstone radars D-622, 1003

Pulse radars D-293

Trinidad, BWI radars D-994

Radio equipment

Hallicrafter type 5x-42 receivers D-257, 258

Philips BX 925-A receiver D-783

Radio-astronomy experimental equipment D-879

Radiometers D-147, 181, 189, 191, 566, 597, 815, 970

Dicke radiometer D-892, 893

Radio polarimeters D-171

Radio sondes D-32

Radio spectrum analyzers D-522

Reflectors, parabolic D-147

Refractors

Schmidt's refractor D-868

Riometers D-48, 470

C. G. Little's riometer D-319

Scintillation counters D-349

Sferic recorders D-482

Solar batteries D-928

Sounding systems

Automatic ionosondes D-283, 441

HF backscatter sounders D-589

Radio sondes D-47

Topside ionospheric sounders D-309

XLVI
Spectrographs D-648

Spectrometers

Radio frequency spectrometers D-333

Spectroscope, dynamic D-903

Survey of U. S. rocket instrumental development D-969

Synchrotrons D-260

Telemetering systems D-693, 840

FM/FM D-969

Pulse-time modulated D-969

SMT D-969

Telescopes (antennas) D-28, 117, 134, 135, 155, 164, 165, 394,

115, 515, 527, 691, 709, 732, 762,

797, 800, 868, 884, 885, 909, 931,

989

Mills Cross D-124, 1007

Pulkovo telescope D-1000

Description of instruments and equipment

Airborne and ground equipment for the upper atmosphere

D-837

Air and space navigation systems/satellites D-496

All-weather sextants D-484, 496

Apparatus for measuring intensity changes/SCNA D-978

Automatic tracking systems/Satellites D-496

D.C. data converter D-969

Delayed repeater satellite transmission systems D-775

Direction finders D-601

Doppler effect recording systems D-696

Electronic enlargers D-686

Equipment for solar eclipses D-734

Equipment for solar observations D-388, 429, 802

Gyro compasses D-595

Interferometers D-442, 683, 709

D. T. M. solar radio interferometer D-597

18 Mc/s wide angle D-875

Swept frequency interferometers D-904

I. G. Y. radio flare detectors D-875

Ionospheric absorption measuring equipment D-631, 658

Magnetic compasses D-595

Maser amplifiers D-248

Measurement systems/I onization D-917

XLVII
Photometers D-686

Polarization systems D-904

Radio receivers

Narrow-band swept receivers D-203

Radio star scintillation spectrum equipment D-901

75-cm receivers D-732

Riometers D-469

Solar noise equipment D-812, 813, 816

Space telemetry systems D-906

Space vehicles D-309, 310

Radio command systems D-999

Solar system reconnaissance vehicles D-116

Space travelling D-32, 642

Bases (future) D-310

Rockets D-264, 333, 337, 374, 375, 403, 517, 533,

619, 624, 642, 647, 668, 721-

723, 837

Lunar rockets D-936

U.S.A. Rockets

Aerobee D-758

HI NRL-50 D-337, 528, 728, 837

No. 20 D-480

No. 24 D-480

No. 38 D-626

Deacon D-758

Juno II D-958

Pioneer II D-695

Pionser III D-253

Pioneer IV D-958

Pioneer V D-219, 238

Viking D-758

V-2 D-480, 721-723, 758, 837

U.S. rocket instrumental development, survey

D-969

U.S. S. R. rockets D-426, 728

Canadian measurements D-961

Rocket equipment D-125, 504

TRAC(E) system D-90

XLVIII
Satellites D-89, 90, 132, 189, 267, 336, 363, 374, 375,

389, 403, 411, 492, 509, 533,

624, 668

U.S.A. satellites

(1958 Ob) Explorer I D-549, 600, 620, 840, 848,

915

(1958 S ) Vanguard I D-125, 198, 389, 390, 602,

620, 907, 928

(1958 r ) Explorer III D-840

(1958 Y ) Explorer IV D-695, 699

(1959 Oi ) Vanguard II D-74, 907

(1959 I ) Vanguard III D-104

(1959 I ) Explorer VII D-7, 415, 473, 481

(1960 # ) Tiros I D-789, 1009

(1961 tf ) Tiros II D-981

Mouse D-759, 845

U.S.S. R. satellites D-42

(1957 4L) Sputnik I D-17, 18, 20, 63, 81, 102,

267, 279, 306, 409, 555, 561,

598-601, 604, 617, 619, 620,

641, 644, 645, 665, 715, 780,

828, 864, 915, 923, 927, 939,

943

(19575 ) Sputnik II D-63, 165, 348, 598, 599,

600, 601, 619, 620, 641, 715,

767, 876, 923, 927, 939, 943

(1958 3) Sputnik in D-6, 87, 131, 176, 233, 238,

239, 262, 279, 333, 404, 414,

425, 427, 471-473, 562, 600-

602, 620, 697, 717, 747, 908,

939, 980, 985, 991

(1959) Lunik I D-993

(1959) Lunik II D-934, 936

United Kingdom satellites

2nd Scout satellite D-949

Satellite-borne instruments D-90, 132, 261, 263, 403, 481,

504, 509, 549, 552, 580, 594,

596, 642, 696, 775, 922, 928,

969, 1006

Infrared sensing elements D-887

Ion traps D-980, 985

Ionospheric sounder-satellite D-835

Radiation sensors D-1006

Telescopes D-775

TV cameras D-789, 981, 1006

XLIX
Aboard

Courier D-755

1958 a D-849

Vanguard I D-198

Antennas D-352, 917

Miscellaneous

Comparison between USA and USSR satellite instrumentation D-761

Equipment to record satellite passages D-153

Satellite hit by micrometeorites D-620

Satellite hit by solar particles D-621

Satellite mapping D-291

Satellite radiation experiments D-981

Satellite weather forecasting possibilities D-291

Sweep -frequency spectrum analyzers D-347

Sweep-frequency sounder-satellite D-835

Sweep recording equipment D-802, 975

Telescopes (antennas) D-347, 351, 396, 410, 513, 686,

750, 800

System for simultaneous image formation D-992

Topside sounders D-961

Wild and Sheridan's spectrum analyzer D-256

Design considerations for:

Artificial navigation systems D-438

Communication satellites D-307

Extraterrestrial communication systems D-62

FM - PM communication systems D-853

Low-noise microwave systems D-771

Meteorological satellite radar systems D-552

Moon relay systems D-736

"Orbiters" D-261

Orbiting astrophysical laboratories D-909

Radio spectrum analyzers D-522

Radiometers D-516

Satellite-borne instrumentation

Aerials at <15 Mc/s D-352

Equipment D-922

Telescopes D-520, 890

Transponding systems D-804
GEOGRAPHICAL OUTLINE

I. HEMISPHERES AND REGIONS

1. Northern Hemisphere D-85, 540, 707

2. Southern Hemisphere D-85, 540

3. Western Hemisphere D-291

4. Polar Regions D-464, 469, 592, 977

North Pole

Polar Cap D-166, 277, 592, 620, 681

Arctic D-311, 467, 554, 681

Norwegian Arctic

Bjornoya (Bear Island) D-482

Soviet Arctic

Tiksi Bay D-977

South Pole

Antarctica

HalleyBay D-85, 86, 554

Scott Base D-959

5. Tropical Regions D-321

Equatorial regions D-402, 508, 987

Equator D-585, 602, 620

6. Temperate Regions D-568

II. CONTINENTS

1. Africa

Congo, Republic of the

Leopoldville - Binza D-295

Ghana

Accra

Achimota D-321, 912

LI
Morocco

Rabat D-100

Nigeria

Ibadan D-632, 912

Sudan

Khartoum D-85, 534, 734, 863

Lake Victoria D-332

Union of South Africa

Cape Town D-250

Grahamstown D-250

Johannesburg D-250

2. Asia

Ceylon D-258

Colombo D-660

Formosa (Taiwan)

Taipei D-315

India

Ahmedabad D-59, 60, 652, 654, 660, 661

Alibag D-491, 764

Baroda D-546

Bombay D-308, 548, 661

Calcutta

Haringhata D-711

Hyderabad D-416

Jabalpur D-246

Jodhpur D-47

Kodaikanal D-151, 162, 450, 851, 951, 965

Madras D-548, 783

Nagpur D-548

New Delhi D-548, 712, 996

Phalodi D-47

Tiruchirapalli D-548

Trivandrum D-660

Waltair D-658, 659

Japan D-329, 330, 346, 548, 838

Hiraiso D-589

Ibaragiken D-591

Kokubunji D-506

Nagoya D-567, 814

Toyokawa D-290, 334, 816

LI I
Sendai D-367

Tokyo D-190, 290, 360, 450

Wakkanai D-334

Malaya

Singapore D-283, 559

Okinawa D-450

Philippine Islands D-653

U. S. S. R. (in Asia) (See also U.S.S.R. under Europe)

Cape Chelyuskin D-425

Irkutsk D-633

3. Australasia

Australia D-123, 128, 330, 350, 654, 709, 903, 940

Cape Hallett D-386

Urisono D-610

New South Wales D-741

Armidale D-77

Canberra D-743

Hornsby D-743

Sydney D-162, 283, 522, 562, 787, 848, 898,

901, 957, 989

Blaxland D-559

Bringelly D-561

Northern Territory

Darwin D-190

Queensland

Brisbane D-88, 743, 880

South. Australia D-208

Adelaide D-207

Camden D-207, 209

Tasmania

Hobart D-190

New Zealand D-13

Dunedin D-ll

Wellington D-ll, 12

LIII
4. Europe

Austria D-169

Freiburg D-671

Belgium

Bruxelles

Uccle D-255

Humain D-255, 397, 579

Manhay D-255, 398

Rochefort D-397, 579

Czechoslovakia

Bratislava D-756

Brasow D-437

Prague D-437

Denmark D-703, 780

Finland D-330

France D-6, 330, 451

Bagneres D-164

Haute Provence D-28

Issy-les-Molineaux D-109

Limours D-35

Meudon D-429, 430, 848

Nancy D-67, 579

Paris D-390, 873

Marcoussis D-177, 178

St. Cyr D-100

Germany D-6, 330, 600, 940

Berlin

Charlottenburg D-862

Potsdam D-436, 716

Bonn D-527, 645

Freiburg D-648

Kiel D-643

Kuhlungsborn D-436, 437, 786

Lindau/Harz D-434, 963

Munich D-390

Ravensburg

Weissenau D-199, 598

Ulm D-598, 601, 602

LIV
British Isles

Great Britain D-150, 330

England D-6, 31, 307, 536, 548, 660,

940, 949, 955

Abinger D-151

Bristol D-299

Cambridge D-63, 151, 706, 773, 848,

873, 894, 908, 909

Dunstable D-595

Farnborough D-63, 620

Harwell D-151

Hull D-299

Hurstmonceux D-151

Jodrell Bank, Cheshire D-85, 117, 118,

120, 122, 154, 155, 165, 476,

511, 565, 579, 651, 686, 773,

958, 972, 989, 1012

Leeds D-151

London D-151, 308, 572-575, 873

Manchester D-797, 873

Portsdown D-389

Rugby D-41

Slough D-42, 43, 63, 87, 559,568,891

Southampton D-299

Yarmouth D-299

Scotland

Aberdeen D-41

Adinburgh D-41, 151

Eskdalemuir D-154, 485

Fraserburgh D-445

Lerwick D-154, 485

Ireland D-842

Italy D-330

Nera D-848

Netherlands D-579

Dwingeloo D-556, 732, 885

Leiden D-989

Norway D-6, 455

trom

Kjeller D-233, 280, 433, 454

Lillestrom

LV
Oslo D-88, 201, 588, 975

Harestua D-203, 693

Tromso D-281, 454, 482, 491

Tromoya D-433

Poland

Warsaw

Jablonna D-482

Spain D-330

Sweden D-6

Goteborg D-458, 796

Kiruna D-268, 319, 472, 473

Stockholm D-449

Uppsala D-791

Switzerland D-330

Jungfraujoch D-216

Payerne D-199

Zurich D-199, 215

U. S. S. R. (see also Asia, USSR) D-350, 390, 403, 619,

641, 715, 750, 755, 939, 988

Azov Sea D-199

Caucasus D-199

Gor'kii D-633

Moscow D-246

Stalingrad D-366

5. North America D-13

Canada D-166, 330, 455, 835

Manitoba

Ft. Churchill D-166, 375, 486, 528, 682,

724, 726

Ontario

Kingston D-702

Ottawa D-67, 146-149, 193, 285, 518, 647,

682, 982

Shirley Bay D-326

Nova Scotia

Inverness D-63, 87, 88

LVI
Quebec

Quebec City D-647

Northwest Territory

Resolute Bay D-166

Saskatchewan

Saskatoon D-230

Cuba D-618

Greenland D-703

Puerto Rico D-994

United States D-330, 482, 509, 536, 581, 639, 686,

755, 800, 831, 835, 844,

876, 887, 890, 940

Alaska D-455, 955

Barrow D-469

College D-48, 326, 445, 464, 469, 636

Ft. Yukon D-48

Arizona D-494

California D-25, 700, 976

Barstow

Goldstone Lake D-90

Mt. Palomar D-868

Palo Alto D-245

San Diego D-444

Stanford D-81, 131, 152, 176, 197, 617,

1013

Colorado D-67, 494

Boulder D-113, 441, 442, 570, 878, 1011

Connecticut

Bethany D-974

District of Columbia D-143, 229, 276, 414,

415, 571, 601, 868, 941,956

Florida D-770

Cape Canaveral D-74, 517, 700, 849, 928,

958

Gainesville D-718

LVII
Hawaii

Maul

Halekala D-677

Idaho D-958

Illinois

Urbana D-962

Iowa

Cedar Rapids D-450

Maryland D-868, 882

Bethesda D-781

Seneca D-931

Massachusetts

Bedford D-26, 601

Boston D-622, 1013

Cambridge D-969

Harvard College Observatory D-67,

956, 957

Hamilton D-7

Sagamore Hill Radio Observatory D-5, 895

Scituate D-2

Westford D-326

Michigan D-272, 375, 924

Nebraska

Ellsworth D-441, 442

New Jersey

Belmar D-180, 962

Ft. Monmouth D-962

Holmdel D-109, 339, 343

New Mexico

Holloman Air Force Base D-494, 626

Sacramento Peak D-175, 522, 714, 902, 926

Sunspot D-218, 714

White Sands D-721-723, 726

New York

Amsterdam D-843

Ithaca D-142, 193, 597, 714, 924

New York City D-781, 843

Schenectady D-26

Troy D-978

LVIII
Ohio

Columbus D-279f 394, 395, 405, 409-

411, 414, 415, 926

Oklahoma D-969

Pennsylvania D-309, 313, 544

Texas D-494, 950

El Campo D-1013

Ft. Davis D-67, 512-514, 830

Utah D-494

Virginia D-882

Ft. Belvoir D-91

Sterling D-450

Washington

Seattle D-152

6. South America

Brazil

Bocayuvo D-534

Chile

Santiago D-276

Peru

Huancayo D-508, 883

7. Oceans and Islands

Pacific Ocean

Eniwetok D-606

Wake Island D-606

VQV

LIX
CHRONOLOGICAL INDEX

1900 - D-474

1923 - D-716

1927 - D-lll

1932 - D-339, 482

1933 - D-340, 341

1935 - D-172, 342

1937 - D-97f 173, 343, 532

1938 - D-100, 790

1940 - D-673

1944 - D-674

1946 - D-29, 30, 150, 181, 299,

607, 704

1948 - D-107, 335, 822, 1001

1949 - D-16, 103, 180, 225, 300,

314, 516, 911

1950 - D-108, 141, 145, 332-

367, 458, 521, 558, 705,

706, 731, 764, 773, 796,

896-898

1951 - D-15, 44, 64, 123, 142,

188, 210, 249, 261, 346,

379, 448, 460, 461, 485,

610, 628, 629, 675, 739,

899

1952 - D-46, 53, 55, 65, 69, 98,

101, 143, 177, 243, 274,

297, 301, 320, 365, 384,

385, 392, 459, 462, 463,

475, 506, 510, 543, 547,

576, 595, 663, 707, 720,

734, 774, 837, 863, 882,

940

1953 - D-41, 114, 162, 178, 179,

184, 185, 195, 211, 321,

338, 361, 418, 419, 429,

480, 541, 545, 548, 630,

669, 721, 749, 812-814,

842, 843, 848, 924, 957,

966

1954 - D-l, 31, 32, 47, 66, 94,

115, 128, 167, 186, 221,

234, 278, 302, 356, 362,

366, 451, 464, 491, 500,

511, 565, 582, 588, 597,

610, 686, 722, 723, 729,

733, 740, 741, 756, 766,

797, 844, 883, 935

1955 - D-22, 28, 33, 34, 45, 52,

68, 70, 105, 212, 218,

223, 232, 235, 246, 257,

269, 284, 285, 289, 298,

303, 330, 351, 358, 363,

370, 376, 405-407, 465,

484, 496, 507, 522, 544,

546, 611, 612, 631, 635,

651, 670, 676, 677, 730,

742, 743, 750, 762, 765,

768, 779, 786, 817, 841,

845, 857, 858, 931, 938,

955, 956, 1002

LX
1956 - D-10, 11, 23, 27, 54, 71,

75, 78, 125, 133, 137,

144, 151, 152, 164, 174,

183, 193, 199, 204, 213,

214, 226, 229, 275, 287,

291, 295, 311, 334, 368,

382, 430, 433, 435, 436,

438, 439, 455, 466, 467,

1958 - (cont'd.) D-783, 795,

804, 816, 832, 834, 838,

849, 854, 876, 877, 880,

894, 904, 910,913, 920,

923, 928, 929, 939, 944,

952, 953, 962, 965, 1010

477, 486, 523, 525, 530, 1959 - D-7, 9, 14, 35, 36, 38,

534, 566, 580, 596, 606, 39, 42, 49, 51, 57, 61-

624, 625, 632, 643, 652, 63, 67, 96, 102, 113,

660, 661, 664, 671, 678, 117-•119, 131, 136, 146,

693, 708, 710, 711, 714, 160, 165, 168, 170, 190,

744, 751, 758-760, 782, 192, 198, 203, 206, 207,

784, 787, 791, 792, 799, 215, 222, 228, 236, 237,

802, 815, 819, 820, 826, 241, 244, 248, 250, 251,

827, 829, 839, 840, 859, 254, 270, 271, 277, 279,

860, 872, 873, 884, 892, 281, 282, 290, 305, 306,

893, 900-903, 912, 921, 309, 318, 319, 323, 327,

922, 926, 930, 937, 941, 336, 350, 360, 364, 369,

946, 951, 954, 979 374, 375, 378, 381, 383,

386, 410, 423, 432, 437,

441, 470, 472, 478, 483,

1957 - D-12, 56, 58, 106, 112, 487, 494, 496, 498, 505,

126, 127, 134, 154-157, 520, 526, 527, 533, 537,

200-202, 276, 280, 312, 552, 553, 556, 559, 562,

313, 331, 337, 344, 371, 567, 577, 581, 584, 585,

372, 380, 447, 450, 454, 587, 589- 591, 601-604,

456, 457, 492, 504, 507, 608, 613, 616, 618, 633,

512, 528, 555, 578, 617, 636, 640, 646, 653, 662,

642, 698, 703, 713, 715, 667, 681, 682, 687, 689,

767, 793, 818, 836, 864, 691, 692, 695, 696, 699,

865, 867, 874, 875, 878, 701, 717, 725, 736, 745,

879, 927, 942, 947, 948, 770, 776, 780, 785, 794,

960, 973, 982 801, 805, 808-810, 828,

833, 835, 846, 847, 851,

861, 862, 868, 870, 871,

1958 - D-469, 499, 501-503, 509, 881, 885, 888, 889, 891,

513, 515, 518, 531, 535, 905, 915, 916, 919, 933,

536, 542, 549, 561, 568, 934, 936, 950, 958, 970,

570, 579, 583, 594, 598, 978

599, 600, 614, 619-621,

623, 626, 639, 641, 644,

645, 657-659, 665, 666,

679, 690, 712, 719, 724,

746, 752, 754, 761, 763,

1960 - D-4, 24, 50, 60, 77, 82,

83-86, 90, 110, 116, 120,

121, 139, 140, 148, 161,

LXI
1960 - (cont'd. ) P-163, 166,

169, 171, 175, 176, 182,

189, 196, 197, 208, 209,

215, 219, 231, 233, 239,

240, 242, 245, 253, 255,

258, 262-264, 268, 283,

294, 296, 307, 308, 315,

322, 329, 333, 352, 354,

357, 377, 398, 411-415,

424, 425, 434, 442, 444,

445, 471, 478, 481, 489,

490, 514, 517, 524, 529,

538-540, 551, 557, 560,

563, 571-575, 586, 592,

622, 627, 637, 638, 648-

650, 655, 656, 668, 680,

683, 685, 694, 697, 702,

718, 726, 732, 737, 738,

753, 757, 769, 771, 772,

777, 778, 789, 798, 800,

803, 807, 811, 821, 823,

830, 831, 850, 852, 853,

855, 856, 866, 887, 890,

895, 906-908, 917, 918,

964, 969, 971, 976, 977,

983, 994, 1011, 1012

1961 - D-5, 6, 8, 21, 25, 26,

43, 48, 74, 76, 89, 91,

93, 95, 99, 104, 109, 122,

132, 147, 149, 153, 217,

224, 230, 238, 252, 260,

266, 288, 292, 293, 316,

317, 325, 326, 348, 355,

373, 387, 391, 393, 401,

404, 417, 426, 443, 453,

473, 488, 493, 497, 519,

550, 554, 564, 569, 593,

609, 615, 634, 647, 654,

672, 684, 688, 700, 709,

727, 728, 735, 747, 748,

755, 775, 781, 788, 806,

824, 825, 869, 886, 909,

914, 925, 932, 945, 949,

959, 961, 963, 967, 968,

972, 974, 975, 980, 981,

984-987, 989-993, 995-

1000, 1003-1009, 1013

1962 - D-310, 988

LXII
BIBLIOGRAPHY ON ATMOSPHERIC ASPECTS

OF

RADIO ASTRONOMY

D-l Aarons, Jules, The solar noise geophysical events relationship. International Council of Scientific Unions, Brussels, Eighth Report of the Commission for the Study of

Solar and Terrestrial Relationships. Paris, 1954. p. 93-97.

25 refs. DWB--Summarizes recent work on "the statistical

study of solar noise - ionospheric disturbances; the eclipse

measurement of radio emissive and optically active solar

centers; and the statistical differentiation between sunspot

groups which produce increases in radio energy and magnetic variations, and sunspot groups which do not. " (Met.

Abst. 9A-45.)--C.E.P.B.

D-2 Aarons, J. and Barron, William R. , Sudden absorption of

atmospherics due to increase in cosmic ray intensity. Nature, London, 178(4527): 277-278, Aug. 4, 1956. fig.,

4 refs. DWB--Atmospheric noise recorded at Scituate,

Mass. , showed a sudden decrease at 0344 U.T. on Feb.

23, 1956, 4 min. after a S.I. D. As the decrease occurred

at night it is attributed to a cosmic ray increase. Noise

returned to pre-absorption level at 0830 U.T. (Met. Abst.

8.3-180.)--C.E.P.B.

D-3 Aarons, J.; Barron, W. R. and Castelli, J. P., Radio

astronomy measurements at VHF and microwaves. Institute of Radio Engineers, N. Y. , Proceedings, 46(1):325-

333, Jan. 1958. 14 figs., table, 5 refs. , eq. DLC--Radio

astronomy measurements of atmospheric absorption, refraction, and scintillation, taken during the summer of 1956

and the spring of 1957, were made at 3. 2 cm and 8. 7 mm

with the sun as the source, and at 218 Mc/s with solar

energy and radiation from Cassiopeia A. Large tropospheric

scintillations at angles below 3 made elevation accuracy

difficult in the 8. 7 mm and 3. 2 cm bands. Refraction at

218 Mc/s was greater than at the microwave wavelengths.

Scintillations at 218 Mc/s were present during periods of auroral activity. The information obtained has been useful in

assessing radar angle-of-elevation accuracy and demonstrates the use of the sun and other celestial bodies as ra- diation sources for antenna pattern measurements. (Met.

Abst. unpub. )- -Authors' abstract.
D-4 Aarons, J.; Castelli, J. P.; Straka, Ronald M. and Kidd,

William C. (all, A. F. Cambridge Res. Center, Bedford,

Mass.), Observations on the solar eclipse of Oct. 2. Nature, London, 185(4708) :230-231, Jan. 23, 1960. 4 figs.,

2 refs. DWB--A preliminary report on the eclipse and scintillation data. Two points are evident from the scintillation

records. First - the shadow patterns at 1300 Mc/s and

3000 Mc/s (generated by the radio frequency active areas

on the sun, which, interfering with one another, normally

decrease the amplitude of the scintillations) are not dependent on frequency. This point is somewhat at variance with

work reported by KAZES (see ref. D-372 ). Second - within

the distance between the centers of the two antennas, a single shadow pattern exists. This latter observation is

generally in accord with work of STEINBERG and KAZES,

(see ref. D- ). (Met. Abst. 11L-313. )--E. Z.S.

D-5 Aarons, J. ; Basu, S. ; Kidd, W., and Allen, R. (all, Air

Force Cambridge Research Lab. , Office of Aerospace Research (U. S. A. F. ), L. G. Hanscom Field, Bedford, Mass.),

Very low frequency modulation of discrete frequency solar

noise bursts. Nature, London, 191(4783): 56-57, July 1,

1961. 4 figs. , ref. DLC--In an effort to study the very-lowfrequency details of different types of solar radio bursts,

observations were made at the Sagamore Hill Radio Observatory, Massachusetts, on three distinct frequencies, 220 M^/s

400 Mc/ s and 3000 Mc/s with an 84_

ft parabolic antenna.

The magnetic tape records, taken to observed d-c to 600

c/s fluctuations, were analyzed over 5-550 c/s to detect

enhancements of absorption in this range. The power spectra of the modulation envelope show that the high-frequency

end of the very-low-frequency band is accentuated. Type II and type III bursts reveal marked attenuation over certain

very low frequency bands. An isolated burst at 220 Mc/s

was associated with a sharp and fast development on a particular band. (Met. Abst. unpub. )--R.B.

D-6 Aarons, J.; Whitney, H. E. (U.S.A.); Roger, R.S. ; Thomson, J. (England); Bournazel, J. ; Vassy, E. (France);

Hess, H. A. ; Rawer, K. (W. Germany); Landmark, B. ; Troim, J. (Norway); Hultqvist, B., and Liszka, L. (Sweden),

Atmospheric phenomena noted in simultaneous observations

of 1958 $ 2 (Sputnik HI). Planetary and Space Science,

5(3): 169- 184, July 1961. 18 figs. , 3 tables, 5 refs. DLC--

Amplitude and Doppler records of the 20 Mc/s-transmissions

of 1958 S 2 (Sputnik III) were simultaneously made at six

radio observatories in Europe. Several distinct phenomena

were noted. A sharp decrease in amplitude, which lasted

from & - lte min and was followed by an abrupt return of the

signal, occurred at the same time at all stations. This

phenomenon has been termed "Dropout, " although indications
of low-level signals were usually present, and is explained

as a sudden decrease in transmitter power of the satellite

perhaps when the satellite passed through a region of high

electron flux. Another type of decrease in the signal was

attributed to highly localized absorbing or scattering regions.

A third phenomenon, recorded by techniques of simultaneous

measurements, was observed in the occurrence of scintillating signals at some stations and Faraday fading at others.

The overlap of the propagation path to each station recording the scintillations defines a vertical slab of ionospheric

region responsible for the scintillations. The region is

about 400-600 km in the horizontal plane but includes small

scale irregularities of less than 1 km. (Met. Abst. unpub.

)

--Authors' abstract.

D-7 Aarons, J. and Castelli, J. P. , Simultaneous scintillation

observations on 1300 Mc and 3000 Mc signals received

during the solar eclipse of Oct. 2, 1959. Institute of Radio

Engineers, N. Y. , Transactions. Antenna and Propagation,

Vol. AP-9(4):390-395, July 1961. (Also issued: URSI Conference (1960). 6 figs., 11 refs. DLC --Very detailed measurements were taken at the USAF Cambridge Research

Center's radio astronomy site at Hamilton, Mass* , using

three radiometers at 224 Mc, 1300 Mc and 3000 Mc. Scintillation of solar signals at 1300 Mc and 3000 Mc basically

is not ionospherically dependent, rather is closely related

to lower atmospheric winds and structure. It is suggested

that the blob structure of the troposphere, possibly at tropopause height, forms into the concave lens focusing the

energy and producing the scintillation. --W. N.

D-8 Acton, Loren W. (Dept. of Astro-Geophysics, Univ. of

Colorado, and Nat. Bur. of Standards, Boulder, Colo. ),

Some relationships between short wave fadeouts. magnetic

chrochets, and solar flares. Journal of Geophysical Research, 66(9):3060-3063, Sept. 1961. 3 figs. , table, 3

refs. DLC --Correlations between the three classes of short

wave fadeouts (S-SWF, slow S-SWF, and G-SWF) and associated magnetic crochets ("solar flare effects* or SFE's) were

examined Jan. 1956 through Dec. 1959. The summarized re- sults, presented graphically and in a table, are discussed

briefly. --W. N.

D-9 Aitchison, G. J. } and Weekes, K. (both. Cavendish Lab. , Cambridge), Some deductions of ionospheric information

from the observations of emissions from satellite 1957 PC 2,

Pt. 1. The theory of analysis. Journal of Atmospheric and

Terrestrial Physics, N. Y. , 14(3/4) :236-243, June 1959.

fig., 2 refs. , 16 eqs. DWB, DLC. Also: Aitchison, G. J. ; Thomson, J. H., and Weekes, K. , Pt. 2, Experimental procedure and results . Ibid., p. 244-248. fig. , 2 tables, 4 refs.
DWB, DLC--The launching of the first artificial earth satellite (1957 <*/) by the U.S.S. R. provided an opportunity of

obtaining information about the ionosphere at heights above

the F2 peak. The satellite emitted radio waves of frequency

20 and 40 Mc/s which were appreciably modified during

their transmission through the ionosphere to the ground. It should therefore be possible to obtain information about the

distribution of ionization by making suitable observations

on the received wave. It turns out that the most useful quantities for this purpose are the Doppler frequency shift and

the fading of the signal caused by the magneto-optical Faraday effect. It is the purpose of the first paper to develop

an approximate theory of these two phenomena and to use it to interpret some observations. Conclusions given in the

second paper are: (1) The analysis of the FARADAY fading

suggests that the ionization density above the maximum of

F2 at night decreases only slowly and that at 100 km above

h F2 it has not decreased by more than 20%. These results are tentative because of the inaccurate knowledge of the

orbit for 1957 0^2 and because the analysis itself is only

approximate. (2) The best Doppler records, although not

sufficiently accurate for detailed analysis, do not appear

to be in disagreement with these conclusions. (3) If full

advantage is to be taken of the information available in the

transmissions from future satellites, it is highly desirable

that accurate orbit data should be available as a result of

visual observations and that records of the Doppler effect

should be made continuously and automatically at several

receiving sites. (Met. Abst. 1 IF-1)--Authors' abstracts.

D-10 Alaska. University. Geophysical Institute, Abstracts of

terrestrial phenomena observed following the solar flare of

Feb. 23, 1956. Paper 03342, 1956. 4 p. mimeo. --Includes

account of cosmic noise absorption. --CSIRO Abstract.

D-ll Allcock, G. McK. and Martin, L.H. , Simultaneous occurrence of "dawn chorus* at places 600 km apart . Nature,

London, 178(4539) :937-938, Oct. 27, 1956. 3 figs. , 3 refs.

DWB--Observations on 273 simultaneous schedules at Wellington and Dunedin, 600 km apart on a geomagnetic meridian, show groups of whistlers on 106 occasions at Wellington and 64 at Dunedin, 56 being simultaneous within 0. 1

sec. Variations with signal strength are shown; the wave

range is less than an octave. (Met. Abst. 8. 2-325)--C. E. P. B.

D-12 Allcock, G. McK. , A study of the audio frequency radio

phenomenon known as "Dawn Chorus. " Australian Journal

of Physics, 10(2): 286 -298, June 1957. 7 figs. , 2 tables,

6 refs. DLC--
Examination of characteristics of "Dawn chorus* as related

to magnetic activity, was conducted at Wellington, New

Zealand, and at other stations during the period July 1955 - Oct. 1956. No correlation with whistlers was found, rather

the experimental evidence favors the hypothesis that "Dawn

chorus" propagated along the lines of the earth's magnetic

field in the extraordinary magneto-ionic mode and apparently

are clouds of positively charged particles of solar origin. -- W.N.

D-13 Allcock, G. McK. (Dominion Phys. Lab. , Lower Hutt, New

Zealand) and Morgan, M. G. (Dartmouth Coll. , Hannover,

N. H. ), Solar activity and whistler dispersion. Journal of

Geophysical Research, 63(3): 573-575, Sept. 1958. 2 figs.

DLC-- Results of regular and simultaneous observations of

whistlers at several locations in North America and in New

Zealand are summarized in graphical form. The results are discussed as contributory evidence for the hypothesis that

the earth revolves within the solar corona; a hypothesis

suggested in 1959 by Ryle and by Chapman, as well as

other research workers. --W. N.

D-14 Allcock, G. McK. (Dominion Physical Lab. , Lower Hutt,

New Zealand), The electron density distribution in the

outer ionosphere derived from Whistler data. Journal of

Atmospheric and Terrestrial Physics, New York, 14(3/4):

185-189, June 1959. 8 figs., table, 13 refs. , 21 eqs.

DWB, DLC--A method, using successive approximations,

is given for finding the variation of electron density N with

height h in the outer ionosphere, when the variation of

whistler dispersion with geomagnetic latitude is already

known. From the application of the method to specific

whistler data, it is inferred that the electron density distribution in the outer ionosphere decreases exponentially

with height at least in the height range 1000 to 13, 000 km,

and that during the period Jan. to May 1957 the equation

describing the distribution within this height range was:

N k 5. 75 x 104

exp (-h/2640) where N is in cm"3 and h in

km.- (Met. Abst. 11F-2) -Author's abstract.

D-15 Allen, C.W. , Observations of solar radio noise. International Council of Scientific Unions, Brussels, 7th Report

of the Commission for the Study of Solar and Terrestrial Relationships, pub. Paris, 1951. p. 63-75. fig. , 3 tables,

54 refs. DWB--Recent observations on 18-35, 000 Mc/s are summarized. Quiet thermal noise, increasing with frequency,

represents an apparent temperature (Ta) of 6400 K at 0. 6 cm.

Steady sunspot noise increases with sunspot area and gives

a maximum at 600 Mc/s, Ta=90 X 106K. On meter wave

lengths there are noise storms, and "bursts" with a line

spectrum. (Met. Abst. 4. 5-116)--C. E. P.B.
D-16 Al'pert, Ia.L., Rasprostranenie radiovolin: spetsializirorannyi biblioqraficheskii spravochnik. (Radio wave propagation: specialized bibliographic reference book. ) Moscow,

Izdatel'stvo Akademii Nauk SSSR, 1949. 195 p. At head

of t-p: Akademiia Nauk SSSR, Otdelenie Fiziko-Matematicheskikh Nauk. DLC --Fifty books are arranged chronologically

by imprint, and over 1500 articles from periodicals are ar- ranged under the following main headings: I. Propagation of

radio waves over the earth's surface (291 refs.); II. Propagation of radio waves in the ionosphere (875 refs.); III. Propagation of the "celestial" ray (199 refs.); IV. Propagation

of ultrashort waves (93 refs.); V. Propagation of radio

waves in the troposphere (57 refs.); and VI. Investigation

on sferics (99 refs.). In some cases, a section is subdivided. References are arranged chronologically within a section (or sub-section). Included are a list of 75 periodicals arranged by country (Russian, England, U.S., France,

Germany, Italy, Japan, Australia, India, and Canada) with

abbreviation and an author index alphabetically arranged.

All titles are in the original language. Imprints cover the

period from 1878-1948. (Met. Abst. 6D-27)--M.L. R.

D-17 Al'pert, Ia.L.; Chudesenko, E. F. and Shapiro, B. S.

,

Rezul'taty issledovaniia vneshnei oblasti ionosfery po

nabliudeniiam za radiosignalami pervoqo iskusstvennogo

sputnika Zemli. (Results of studies conducted in the outer

regions of the ionosphere by observations of radio signals

of the first artificial earth satellite. ) Akademiia Nauk

SSSR. Mezhduvedomstvennyi Komitet po Provedeniiu MGG,

Predvaritel'nye itogi nauchnykh issledovanif. . . sputnikov

Zemli i raket. No. 1:40-108, 1958. 18 figs. , 26 tables,

15 refs. , 28 eqs. English summary p. 51. DWB--The

method of research on the upper atmosphere by means of

artificial earth satellites described in this paper is based

upon the determination of the time of "radios et" and "radiorise" of the satellite. The distribution of the concentration

of electrons in the outer ionosphere provides information

about the properties of interplanetary gases. The trajectories of radio waves in the ionosphere and methods of investigating them are described in detail. Results of the

theoretical calculations of the maximum horizontal distance

of the receipt of radio signals are given. The calculations

were made for a spherical earth, and the tabulation of the re- sulting elliptical integrals was carried out with a high-speed

electronic computer. The calculations used the parabolic

model of the lower ionosphere and the exponential decrease

of the electron concentration in its outer part. In the analysis of the experimental data, the parameters of the lower

ionosphere and the altitude of the artificial satellite were
used and the maximum distances of signal reception were

determined on the basis of ballistic data and other studies

of the trajectories of the satellite. The electron concentration of the ionosphere N was found to decrease much slower

after its maximum Nm than it increased to the maximum Nm. For the model N ^N e"

XZ

, the value X^ 3. 5 10"3 1/km

z m

is obtained. This means that the number of electrons in the

outer part of the ionosphere is approximately 3. 6 more than

in the lower part. Extrapolation of the observational data

received for the altitudes z ^300-^ 650-700 km to z^3000

shows that with z ~ 2000 - 3000 km, N ^ 200 - 300 el/cm3. A curve of the density of neutral particles n(z) according to

the lifetime of the electron and the time between different

acts of ionization is drawn. It is concluded that the altitude of the "limits* of the atmosphere (region of contact with

interplanetary space) is of the order of 2000 - 3000 km. Appendices contain the following: calculation of the maximum

distance of distribution of waves in the approximation of

geometrical optics and tables of maximum horizontal distance rm (in km) for a series of given parameters. Met.

Abst. 11E-7) -Authors' abstract and I.L.D.

D-18 Al'pert, Ia.L.; Dobriakova, F. F. et al. , O nekotorykh

rezul'tatakh opredeleniia elektronnoi kontsentratsii vneshnei oblasti ionosfery po nabliudeniiam za radiosiqnalami

pervoqo sputnika Zemli . (Some results of determining the

electron concentration of the outer region of the ionosphere

from observations of the radio signals of the first earth satellite. ) Uspekhi Fizicheskikh Nauk, Moscow, 65(2):161-

174, 1958. 9 figs. , 28 eqs. DLC--Sputnik I broadcast at

40 Mc/s allowing calculations to be made of the electron

concentration in the layers of the ionosphere by measuring

the time of rising and setting of the satellite radio beam.

Results of observations made at 6 places on Oct. 5, 6, and

7, 1957, are tabulated and analyzed. Methods of determining the radio paths in the ionosphere are reviewed from theoretical and practical viewpoints; then the details of calculating the distance of the object at the time of radio rising

and setting are presented mathematically and graphically;

followed by results of such analysis and, finally, a discussion of analysis of the determined electron concentration of

the outer ionized layers and density of interplanetary gas

(320 to 2450-km height). (Met. Abst. HJ-3)--M. R.

D-19 Al'pert, Ia.L., Ionosfera i iskusstvennve sputniki Zemli. (The ionosphere and artificial earth satellites.) Priroda,

Moscow, No. 10:71-77, Oct. 1958. 3 figs. DLC--
The author discusses the pre-Sputnik knowledge on the concentration and density of electrons above the earth and the

importance of more precise data on the distribution of electrons with altitude above 100 km, the effective frequency of

collisions of electrons with other heavier gas particles, and

the small-scale inhomogeneities in the atmosphere. The

possible origins of these inhomogeneities, which are characterized by fluctuations of electron concentration, are considered, namely: ionospheric turbulence and longitudinal

plasma waves. The special problems arising in the use of

satellites to study the atmosphere are considered. These

result from the use of radio signals to measure various parameters and the complexity of effects occurring in the vicinity

of the satellite. The applications of the coherent Doppler

method and of the method of observation based upon radio

"rise" and "set" are discussed. (Met. Abst. 10. 10-200)--I.L. D.

D-20 Al'pert, Ia.L., Sostoianie vneshnei ionosfery. (The state

of the outer ionosphere. ) Priroda, Moscow, No. 6:86-87,

June 1958. table, 3 foot-refs. DLC. Trans, into English

by E. R.Hope issued as Canada. Defence Research Board

Translation T-304-R, Sept. 1958. DWB--The method of radio

observations on the first earth satellite is described briefly

and the results of such observations at 6 points during Oct.

5, 6,and 7, 1957, are summarized. The electron concentration in the outer ionosphere diminished with altitude considerably more slowly than it increased in its lower portion.

q

A table is presented giving the electron concentration N/cm

up to 3100 km and also the density of neutral particles per

3

cm up to the same height. The computation of the density

of the latter is described. At distances of 2000-3000 km

from the earth, the electron concentration is close to

3 2 3

10 -10 electrons/cm and the density of neutral particles

is of the order of 1 per/cm . Hence the atmosphere approaches the properties of interplanetary gas at 2000-3000

km. The agreement between the data on the outer atmosphere obtained by means of rockets and lunar signals is

compared with those obtained with the artificial earth satellite. (Met. Abst. 10. 10-20D--I.L.D.

D-21 Al'pert, la. L. , Investigation of the ionosphere and of the

interplanetary gas with the aid of artificial satellites and

space rockets . Soviet Physics USPEKHI, N. Y. , 3(4):479-

503, Jan. /Feb. 1961. 27 figs. , 49 refs. , 61 eqs, DLC.

Transl. of -original Russian by J. G. Adashko in Uspekhi

Fizicheskikh Nauk, Moscow, 71(3/4) :369-407, July 1960.

DLC --Several methods of investigating the electromagnetic

properties of the ionosphere and the interplanetary gas, by

means of rockets and satellites, are discussed. The

8
introduction contains a summary of experimental results,

reviews the research problems and outlines approach for

attack. The Doppler effects at radio frequency are treated,

also the amplitude characteristics of radio signals from

rockets and satellites. The satellite produced plasma perturbations are taken up next and systematically discussed

in relation to sub-subjects under the above mentioned main

topics. The development of radio and engineering methods,

well organized in practical and theoretical aspects, will

yield knowledge about the physical nature of the ionosphere

and the space beyond. (Met. Abst. unpub. )--W. N.

D-22 American Geophysical Union. Special Committee on CosmicTerrestrial Relationships, Report of the Committee, 1954-

1955. Harlan T. Stetson, chairman, American Geophysical

Union, Transactions, 36(6): 1061-1066, Dec. 1955. 18 refs.

DWB, DLC -Reports by HELEN DODSON, D.H.MENZEL,

E.O.HULBERT, H.W.WELLS, HERBERT RIEHL, E.M.

BROOKS and S.A.KORFF cover investigations in fields of

basic solar research (solar flares, etc. ), solar-ionospheric

relationships, radio-astronomy of sun, rocket ionospheric

and UV solar spectrum studies, whistling atmospherics,

cosmic rays, rainfall variations due to cosmic influences,

and temperature variations with sunspot cycle. (Met. Abst.

8.3-46.)--M.R.

D-23 American Geophysical Union. Special Committee on CosmicTerrestrial Relationships, Report for the year ending June

30. 1956. Harlan T. Stetson, chairman. American Geophysical Union, Transactions, 37(4) :491 -496, Aug. 1956. 23

refs. DWB, DLC --Reviews are given of solar research by

the Harvard Observatory and by the McMath-Hulbert Observatory, the work on radio astronomy, the upper atmosphere,

solar radiation and audio-frequency atmospherics by the

Naval Research Laboratory on relationship between solar

activity and meteorological changes, on sunspot-weather

correlations and on solar energy exchange in the atmosphere.

(Met. Abst. 9A-102. )-I.L.D.

D-24 Anderson, D.S., Ionospheric studies from an analysis of

satellite radio signals with an automatic tracking filter . Pennsylvania State Univ., Ionosphere Research Lab. , Contract AF 33(616) -6157, Scientific Report No. 138, Sept. 1,

1960. 58 p. 15 figs, (including photos), 4 tables, 14 refs.,

numerous eqs. DWB--A brief survey is made of the methods

used for ionospheric investigation. This includes a simple

illustration of the theory of the dispersive Doppler experiment utilizing radio transmissions from earth satellites. Detailed descriptions of the equipment used to measure the dispersive Doppler frequency are given. In particular, an
automatic tracking filter which was especially designed for

this study is discussed. A preliminary study was made of

data obtained utilizing this equipment. The primary data

consists of total electron content, from which a thickness

parameter was derived. The factors which influence this

parameter were investigated and the results are reported.

(Met. Abst. 11. 12-366. ) -Author's abstract.

D-25 Anderson, Lloyd J. (Smyth Res. Associates, San Diego,

Calif. ), VHF satellite signals received at extra optical

distances. Institute of Radio Engineers, New York, Proceedings, 49(5):959-960, May 1961. 2 figs. DLC--Low

angle refraction of radio waves, using 108, 162, and 216

Mc/s satellite signals, were experimentally measured in

California June-Aug. 1960. The signals in most cases were

received while the satellite was beyond the radio horizon;

in two cases 1700 - 1900 miles beyond. No consistent frequency dependence, low attenuation and control radiosonde

data favorably support a tropospheric ducting mechanism

suggested. (Met. Abst. unpub. )--W. N.

D-26 Anderson, Roy E. (General Electric Co. General Eng. Lab.,

Schenectady, N. Y. ), Sideband correlation of lunar and

echo satellite reflection signals in the 900 Mc range. Institute of Radio Engineers, N. Y. , Proceedings, 40(6):1081-

1082, June 1961. 2 figs. , table, 3 refs. DLC -The results

of lunar reflection tests, as conducted by General Electric 's Radio-Optical Observatory near Schenectady, N. J. , and at

Air Force Cambridge Research Lab. , Bedford, Mass. , are presented and discussed. The moon was illuminated at 915

Mc using double side band suppressed carrier modulation,

reflectionsof which were received with a 28-ft antenna located at Schenectady. Amplitude fluctuations over the path

were also measured. Correlation coefficients, using a digital computer, are tabulated and characteristic moon echo re- cords reproduced. (Met. Abst. unpub. )-- W.N.

D-27 Andre, Pierre; Kazes, Ilya and Steinberg, Jean-Louis,

Mesure de 1 'absorption atmospherigue sur 9350 Mhz utilisant

le rayonnement radioelectrigue solaire. (Measurement of

atmospheric absorption at 9350 Mc/s using solar radioelectric radiation. ) Academie des Sciences, Paris, Comptes

Rendus, 242(17): 2099-2101, April 23, 1956. fig. , 4 refs.

,

2 eqs. DLC--Solar radiation at 9350 Mc/s undergoes an attenuation while the sun is setting. Only a part of this attenuation can be attributed to absorption by atmospheric

oxygen and water vapor, a residual 35% remaining unexplained. (Met. Abst. 9A-103. )-- Trans, of authors' abstract.

10
D-28 Andrillat, Henri, Les temperatures electroniques des

nebuleuses planetaires . (Electronic temperature of planetary nebulae. ) Annales d'Astrophysique, Paris, Supplement, No. 1, 1955. 58 p. 11 figs. , 20 tables, 51 refs.

,

eqs. DLC, DWB—A detailed monograph giving the complete results of studies of the physics of planetary nebulae

based on data for 24 nebulae obtained at Haute Provence

Observatory (electronic temperature of 8000 to 27, 000

were obtained) with a 120 cm telescope. Theory is reviewed

in Pt. 1; in Pt. 2 the spectrophotometrically determined temperatures (methods, sources of error, accuracy, and comparison of results with those of other authors) are treated. On

p. 20 the correction for atmospheric absorption, and on p.

21,- for atmospheric dispersion, are discussed. Finally, the

intensity of rays of hydrogen, helium, and (O III) at 5007 A

is covered. In Pt. 3, continuous and discontinuous Balmer

spectra of gaseous nebulae are treated (atmospheric absorption and dispersion on p. 43). Met. Abst. 11. 6-77. )--M. R.

D-29 Appleton, Sir Edward and Hey, J. S. , Solar noise. I. Philosophical Magazine, 37(265) :73-84, Feb. 1946. 5 figs.,

table, 9 refs. , 4 eqs. DLC --Based on evidence discussed,

it is concluded that the radar-observed noise is propagation

of electromagnetic waves from the sun, and not originated

from violent perturbations of ionization in the ionosphere.

The noise has been observed associated with solar flares

and SWF's. --W.N.

D-30 Appieton, Sir E. and Hey, J. S. , Circular polarization of

solar radio noise. Nature, London, 158(4010):339, Sept. 7,

1946. 3 figs. --In this very brief note reference is made to

earlier observations of 5 V\, from sunspot areas. Experimental examination of solar radio noise at 85 Mc/s during sunspot activity (July 27 and 28, 1946) showed a circular lefthanded polarization. The connection with local solar magnetic field is thus apparent. --W. N.

D-31 Appleton, Sir E. and Piggott, W. R. , Ionospheric absorption measurements during a sunspot cycle. Journal of Atmospheric and Terrestrial Physics, 5(3):141-172, July 1954. 16

figs. , 3 tables, 26 refs. , 38 eqs. DWB--The results of measurements of absorption of radio waves in ionospheric reflection, made in S. E. England 1935-1953, are examined, [log hj

( P = effective reflection coefficient) is related to radio

wave frequency f, solar zenith distance X, and sunspot

number R. Variation with f is accounted for by magnetoionic theory. £log p]Jis proportional to (cos X)0. ^5 instead

of (cos X)l* 5 as simple theory predicts, but with occasions

of excessive absorption on winter days associated with

sporadic reflection below E layer. There is a direct relation

11
with Rf especially in summer. The absorbing layer is believed to be within D layer. It is probable that sudden

ionospheric disturbances associated with solar flares are due to ionization increased 5-10 times in the normal absorbing layer (level of D layer) but D layer does not contribute

substantially to diurnal magnetic variations. (Met. Abst.

5. ll-66.)--C.E.P.B.

D-32 Appleton, Sir E. , Finding things out with radio and rockets.

Advancement of Science, London, 10:355-364, 1954. GB-MO

--Good popular account of exploration of the atmosphere by

balloon, radiosonde and rocket (mainly determination of temperature stratification) and of the ionosphere by radio pulses

of different frequencies. Author continues with information

from solar radiations and meteors, and ends with a discussion of the possibility of space travel. (Met. Abst. 6. 9-84)

--C E. P. B.

D-33 Appleton, Sir E. , Rocket sounding in the upper air: confirmation of results inferred from radio measurements . Wireless World, London, 61(9). 406-407, Sept. 1955. 4 eqs.

DLC--In connection with plans for the International Geophysical Year, the article briefly describes methods of measuring pressures and deducing temperatures, and of measuring

electron density at a given height by the Doppler effect on

the phase velocity of radio waves near the rocket emitter.

(Met. Abst. 12E-77.)-C.E.P.B.

D-34 Appleton, Sir E. and Beynon, W. J. G. , An ionospheric

attenuation egiuvalence theorem. Journal of Atmospheric

and Terrestrial Physics, 6(2/3): 141-148, March 1955. 2 figs.,

8 refs. , 21 eqs. DWB--The phenomenon of radio wave attenuation by way of ionospheric partial reflections and scattering is examined theoretically, and an equivalence theorem,

relating oblique incidence to vertical incidence phenomena,

is derived. For radio frequencies well in excess of the equivalent critical frequency of the medium this may be written

r i.r f * r i f cos ^0

where p is the fractional attenuation, f is the frequency,

and i the angle of incidence in the oblique incidence case.

Where the radio wave electric vector is at right angles to

the plane of propagation, S\ is unity; when the electric

vector lies in the plane of propagation, A is equal to the

usual obliquity factor cos 2 i . (Met. Abst. 6D-272. )--

Authors' abstract.

12
D-35 Armier, G. , L'ecoute des satellites artificiels au centre

R. T. F. de Limours. (Monitoring of artificial satellites at

theR.T.F. station at Limours. ) L "Onde Electrique, Paris,

39(388/389) :654-659, July/Aug. 1959. 5 figs., 2 tables.

DLC--The article is divided into two parts: a) The monitor- ings: durations, sub-division, statistics, influence of or- bital position, abnormal propagation; b) Measurement of

frequencies. Emphasis is placed on the special details of

the equipment used for 20 Mc/s. The method is completely

automatic, the only adjustment is that of setting the re- ceiver on frequency. A counter automatically records the

frequency shift. The accuracy of one cycle is obtained for

signals of less than 1 microvolt at the input of the receiver.

The maximum speed of operation is about one complete measurement of frequency every 2 seconds. The study is concluded by the analysis of some curves showing frequency

shift due to Doppler effect. (Met. Abst. 11. 12-567.)--

Author's abstract.

D-36 Astronomical Society of the Pacific, Abstracts of papers

presented at the San Francisco meeting ..... June 17-18.

1959. Astronomical Society of the Pacific, San Francisco,

Publications, 71(422): 381-393, Oct. 1959. fig., 2 refs.

DLC --Abstracts of 13 papers. Following are the titles of

the papers: 1) Radar studies of the cislunar medium, 2)

Recent tests with image tubes; 3) Orbits for planetary satellites from Doppler data alone; 4) The orbit of the spectroscopic binary tauri; 5) Satellite studies of outer atmospheric ionization; 6) Electric power for lunar stations; 7)

An image-tube experiment at the Lick Observatory; 8) Sensitive detectors for radio astronomy; 9) Galactic orbits of

stars; 10) The orbit and spectrum of HO 95635; 11) Whistlers in the extraterrestrial environment; 12) Magnetic compression in the geomagnetic field as measured by Pioneer I; 13) Spectroscopic investigations of multiple galaxies and

clusters of galaxies. (Met. Abst. 11L-1. )--I. S.

D-37 Avignon, Yvette; Boischot, A. and Simon, P. (all, Observatory of Meudon), Caracteres d'une emission solaire

remarquable observee le 4 novembre 1957 sur 169 MHz.

(Characters of a remarkable solar emission, observed on

Nov. 4, 1957 at 169 Mc/ s ) Annales d'Astrophysique,

Paris, 21(5): 243-249, Sept. /Oct. 1958. 6 figs., 3 refs.

English and Russian summaries p. 243. DWB, DLC --On

Nov. 4, a very exceptional solar emission was observed

at 169 Mc/s. Its unusual characteristics were very different than the ones characterizing noise storms and bursts

generally associated with chromospheric flares. It is suggested that some of the observed fluctuations originated in a seeing phenomenon close to the earth. (Met. Abst.

10. 10-85. )- -Authors' abstract.

13
D-38 Avignon, Y. and Pick, Monique, Relation entre les emissions du type IV et d'autres formes d'activite solaire.

(Relationship between type IV emissions and other forms

of solar activity. ) Academie des Sciences, Paris, Comptes

Rendus, 248(3) :368-371, Jan. 19, 1959. fig. , table, 9

refs. DWB, DLC--Type IV emissions defined on metric

waves are generally associated with large jumps on centimetric waves. It is shown that a slight connection exists

between optical centers which give rise to type IV and

centers of radioelectric storms. The frequent occurrence

of two or three optical centers, giving several type IV's

during the same period is also shown. (Met. Abst. 11. 5-

153.)--A.V.

D-39 Avignon, Y. and Pick, M. , Relation entre les emissions

solaires de rayons cosmiques et les sursauts du type IV . (Relationship between the solar emissions of cosmic rays

and the Type IV jumps.) Academie des Sciences, Paris,

Comptes Rendus, 249(22): 2276-2278, Nov. 22, 1959. fig.,

8 refs. DWB, DLC--A close relationship between the Type

IV jumps of radioelectric radiation with intensity superior

to a determined energy on the one hand, and the increase

of cosmic radiation observed near the ground on the other

hand, is established, taking into account the heliographic

coordinates and the importance of the associated optical

eruption. From this relationship it is inferred that an eruption probably produces cosmic rays observable near the

ground when its importance is equal to 3 or 3

+

, while cor- responding to a jump of Type IV superior to 5 and when

situated in the western part of the solar disk. The close

relationship between Type IV jump and solar cosmic rays

proves that the measurement of the importance of Type IV

through its radiation in the field of the centimetric waves

is very significant. (Met. Abst. 11. 5-154. )--A. V.

D-40 Bailey, V. A. (U. of Sydney, Australia) and Goldstein, L.

(U. of 111. ), Control of the ionosphere by means of radio

waves. Journal of Atmospheric and Terrestrial Physics,

London, 12(2/3):216-217, 1958. 8 refs. DLC--As a radio

wave traverses an ionized gas, consequently raising its

temperature, energy is produced. But in the absence of

some source of ionizing energy the gaseous plasma disappears. Radio waves of sufficient intensity affect the ionization produced by solar radiation or other agencies in any

region of the ionosphere, even when the temperature is as

low as 250-300 K. When a rise in temperature has changed

the rates of different processes of diffusion, attachment and

recombination ionization can still be controlled by the es- tablishment of radio stations on the ground, especially when

the controlling waves have their frequencies near the gyrofrequency of electrons in the ionospheric region concerned.

(Met. Abst. 10. 6-171. )-N. N.

14
D-41 Bain, W. C. , Observations on the propagation of very long

radio waves reflected obliquely from the ionosphere during

a solar flare. Journal of Atmospheric and Terrestrial Physics, 3(3):141-152f April 1953. 6 figs. , table, 19 refs.

MH-BH--Describes measurements of amplitude and phase of

16 kc/s sky wave, Rugby to Aberdeen. Normal diurnal variation of apparent height of reflection at normal and oblique

incidence is shown and sudden field anomalies at Aberdeen

and Edinburgh during solar flares illustrated. It is found

that during a moderate flare with large zenith distance of

sun there is a change of apparent reflection height for vertical but not for oblique incidence. Phenomena are attributed to a double structure of D layer, the lower layer (at

70 km) being responsible for oblique incidence propagation

(including atmospherics)and the upper affected by solar

radiation during a flare. (Met. Abst. 5. 6-284. )--C. E. P. B.

D-42 Bain, W.C. and Shearman, E. D. R. , Observations on the

U. S.S. R. earth satellites and the study of radio wave propagation. Institution of Electrical Engineers, Proceedings,

Pt. B, 106(27): 259-263, May 1959. 5 figs., table, 8 refs.

,

3 eqs. DLC --Measurement of bearing, angle of elevation

and Doppler frequency shift have been performed at Slough

on transmissions from the Russian earth satellites. The

examples considered here indicate that the observed phenomena can be accounted for satisfactorily in terms of our present knowledge of ionospheric propagation. A short

section is included on orbital determination from the measurements. (Met. Abst. 11E-13. ) --Authors' abstract.

D-43 Bain, W.C. (Radio Research Station, D. S.I. R. , Slough),

Irregular fading of satellite transmissions. Nature, London,

189(4759): 129, Jan. 14, 1961. table, 2 refs. DWB-It has

been suggested that the fact that irregular fading of satellite transmissions on 40 Mc/s from Sputnik I were not observed at Cambridge when satellite was south of 50 N was

due, not to the absence of irregularities south of Cambridge, but to the southerly irregularities being incorrectly

orientated to give appreciable power scattering to the re- ceiver. Observations made at Slough on transmissions

from Explorer 7 at a frequency of 20 Mc/s show frequent

occurrences of irregular fluctuations although the satellite

never reaches as far north as Slough. (Met. Abst. unpub.

)

--R.B.

D-44 Baldinger, E. and Schaetti, N. , 9. Generalvers ammlunq

der Union Radio-Scientifique Internationale (U. R. S. I. ) in

Zurich (vom 11. -22. September 1950). (Ninth general meeting of the International Scientific Radio Union (U. R.S.I.)

in Zurich (Sept. 11-22, 1950).) Zeitschrift fur angewandte

Mathematik und Physik, 2(3):212-214, May 15, 1951. MH-BH

15
A brief report of the meeting including recommendations for

further investigations to the following Commissions: II. Propagation in the troposphere (further investigation of influence of latitude, nature of ground and climate on refractive

index, especially for short waves); III. Ionosphere and propagation of waves; IV, V. Radio noises of terrestrial origin

and of extraterrestrial origin. (Met. Abst. 5.6-285.)--

C. E. P. B.

D-45 Banerjee, D. K. ; Surange, P. G. and Sharma, S. K. (all,

Engr. Col. , Banaras Hindu Univ. ), Ionospheric observations at Banaras during the total solar eclipse on June 20.

1955. Journal of Scientific and Industrial Research, Sec. A,

14(11):517-521, Nov. 1955. 5 figs. , 17 refs. DWBObservations of intensity of radio signals on 30. 5 and 30. 7

m from Colombo and Delhi were made at Banaras during the

total eclipse at Colombo, to see what effect the totality had

on the ionosphere. Oblique and vertical incidence measurements gave data on variations in field strength, electron

density, semithickness and height of lower boundary of F2

layer. Conclusions were: 1) duration of eclipse is less

than that of ionospheric eclipse; 2) effect of absorbing re- gions in lower ionosphere is more pronounced in the eclipse

area than at Delhi; 3) field strength of Colombo signals increased and at Delhi decreased during eclipse. Finally, it

was concluded that the sudden increase in solar radiation at

end of eclipse produced thermal expansion of the ionized

layer. (Met. Abst. 7. 11-290. )--M. R.

D-46 Banerjee, S. S. ; Rajan, V. D. and Banerjee, P. C. (Benares

Hindu Univ. ), Some observations on the effect of solar

eclipse on the F2 region of the ionosphere. Journal of Scientific and Industrial Research, New Delhi, 11B(5): 197-198,

May 1952. fig., 7 refs. DWB--An analysis of observations

made with short wave radio signals both at the vertical and

oblique incidence during the solar eclipse at Benares on Feb.

28, 1952, in order to determine the source of ionization in

the F2 region. Evidence is presented indicating the possibility that the ionization in the F2 region observed during the

eclipse is due to neutral particles emitted by the sun. (Met.

Abst. 4.4-93.)-I.L.D.

D-47 Banerjee, S. S. , The solar eclipse of June 30, 1954. Science and Culture, Calcutta, 20(l):2-3, 34, July 1954.

DWB--Observations made at Phalodi, India (70 mi NW of

Jodhpur) during the 1 min 8 sec of totality and for several

days before and after the eclipse of June 30, 1954, are described. These include solar, ionospheric, radio noise, geomagnetic, eye, atmospheric electric potential gradient and

conductivity, and ordinary meteorological observations at the

16
surface and in the upper atmosphere by means of special

and normal radiosondes. (Met. Abst. 6. 6-323. )--M. R.

D-48 Easier, Roy P. , The aurorally associated ionospheric absorption of cosmic radio noise. Alaska. Univ. Geophysical

Institute, NSF Grant G 14133, Scientific Report No. 1, May

1961. 63 p. 13 figs., 2 tables, 25 refs. , eqs. DWB

(M(051) A323sct)--The riometer records of 27.6 Mc/s cosmic

noise from the Alaskan IGY stations are used to study the

phenomenon of aurorally associated absorption. The emphasis of the work is on the comparison of the auroral absorption recorded at different latitudes, and the primary re- sult is the definition of an auroral absorption zone. This

zone is compared to the analogous visual auroral zone, and

the geomagnetic latitude of. maximum intensity of the absorption zone is found to be near College (64,65 ) whereas

the latitude of the peak of the visual zone is near Ft. Yukon

(66.69 ). The auroral absorption zone is more pronounced

during magnetically disturbed periods, but daily and seasonal variations are generally the most effective secondary

factors determining its character. Absorption is found to

exhibit a daytime maximum at all stations, and a winter

maximum in auroral absorption is observed at College. Possible interpretations of the discrepancy between the absorption and visual zones are suggested in terms of the relation

of these zones to the primary auroral particles. --Author's

abstract.

D-49 Bauer, Siegfried J. and Daniels, Fred B. (both, U.S. Army

Signal Res. & Dev. Lab., Ft. Monmouth, N.J,), Measurements of ionospheric electron content by the lunar radio

technique. Journal of Geophysical Research, Wash. , D. C.

,

64(10):1371-1376, Oct. 1959. 7 figs., 9 refs. , eqs. DLC--

Measurements of the Faraday rotation of lunar radio echoes

on a frequency of 151 Mc/s are used to determine the time

variation in the total ionospheric electron content. Absolute values of ionospheric electron content are determined

from these measurements in conjunction with information on

the electron content below the F2 peak computed from verti*-

cal incidence sounding data. Diurnal, day-to-day, and seasonal variations in the total electron content are presented.

The ratio %&, ' ^t, of the number of electrons above the F2

peak to that below is found to be in the order of 4 to 5 during three summer nights (June) before sunrise and about

equal to 3 after sunrise. For two days in Nov. the ratio

l^a. '• ^ b is found to be equal to about three both before

and after sunrise. Possibilities of inferring other characteristics of the upper ionosphere from observed variations in

the total electron content are briefly discussed. (Met. Abst.

11F-9. )--Authors' abstract.

17
D-50 Bazzard, G.H. (DSIR Radio Res. Station, Slough), Shortterm differences in the behaviour of two daily indices of

solar activity during the IGY. Journal of Atmospheric and

Terrestrial Physics, London, 18(4): 290-296, Aug. 1960.

2 figs., 4 tables, 13 refs. , eq. DLC—The variations in the

daily values of the flux of solar radio noise at A. 10. 7 cm

(I? ) and the E, layer character figure (J-,) have been studied

for the period of the IGY. It is found that <£ lags behind

J-. by about 14 hrs. The ratio 1-e/ § fluctuates above and

below its normal value, and the reasons for these changes

have been examined. Troughs in J^/l? are attributed

partly to increases in geomagnetic activity which cause a decrease in JL, and partly to the presence of active regions

on the sun's disk which tend to emit relatively more radio

noise than the quiet sun. Peaks in Jw/«£ are associated

with the absence of these active areas. (Met. Abst,

11. 12-45)--Author's abstract.

D-51 Beckmann, B. , First results of satellite observations for

information. Nachrichtentechnische Zeitschrift, 12:335-343,

July 1959. Unchecked. --A review of earlier radio and radar

observations of earth satellites, and a summary of results

obtained relating to ionospheric phenomena are given. -- IRE Abst. 3495.

D-52 Beer, Arthur (ed. ), Vistas in astronomy. London, Pergamon Press, 1955. 2 vol. (Vol. 1, 776 p. Vol. 2, p. 779-

1770). figs. , tables, refs. , bibliogs, eqs. Indexes in

Vol. 2. (Special Supplements, No. 3 and 4, to the Journal

of Atmospheric and Terrestrial Physics). DLC (QB3.B35),

DWB (520. 82 B415v). Review by H. H. Voigt in Die Naturwissenschaften, Berlin, 45(17) :427, Sept. 1, 1958. Review

by B. Vorontsov-Vel'iaminov in Astronomicheskii Zhurnal,

Moscow, 35(3):496-498, May/June 1958. -Vol. I of this

series of "Compendiums" on astronomy and astrophysics included 7 sections: organization, history, dynamics, theory,

instruments, radio astronomy, and solar physics. The second

volume covers sections 8-16 (including 100 articles by authorities): solar-terrestrial relations, geophysics, planetary

systems, stellar astronomy, photometry, spectroscopy,

novae, galaxies, and lastly, cosmogony and cosmology.

The section on solar-terrestrial relations (p. 779-826) contains 6 articles on the ionosphere (SIR EDWARD APPLETON),

absorption of radio waves in the ionosphere (J. A. RATCLIFFE),

solar flares (M.A.ELLISON), M-regions and solar activity

(M.WALDMEIER), the corpuscular radiation of the sun

(M.J.SMYTH), and solar cosmic rays (P.M.S.BLACKETT).

In the section on geophysics there is an article on thunder18
storm (E.T.PIERCE), atmospheric C02 (LEO GOLDBERG), infrared spectrum of atmosphere (T. W. WORMELL), the 0~ layer

and the 9. 6 ^ 3 band (R. M. GOODY and CD. WALSHAW),

0~ near the North Pole (A. E. DOUGLAS et al. ), upper atmosphere rocket soundings (S. F. SINGER ), geomagnetic storms and

bays (SYDNEY CHAPMAN), and the airglow (DANIEL BARBIER).

In the section on the planetary system, LUIGI G. JACCHIA and

F.L. WHIPPLE have an article on the Harvard photographic meteor program, MIROSLAV PLAVEC has one on the evolution of

meteor streams, and H.C. VAN de HULST has one on the zodiacal light. Finally, in the last section (16) F.A.PANETH has

an article on the frequency of meteoritic falls through the ages,

and HAROLD C.UREY one on the origin and properties of the

moon's surface. Each article is abstracted separately and will

be run in later issues of MAB. Extensive bibliographies ac- company many of the articles, and illustrative material in the

form of diagrams, photographs and tables are interspersed

throughout the text. (Met. Abst. 10. 10-6. )--M. R.

D-53 Behr, A. and Siedentopf, H. , Sonnenuberwachung. (Solar

Survey.) Naturwissenschaften, 39(2):28-38, Jan. 1952. 13

figs. , 3 tables, 20 refs. DWB--The various sources and types

of radiation from the sun, and their terrestrial effects are summarized in a diagram. Types, distribution and variations of

sunspots are described, then faculae, eruptions, protuberances

and filaments. Observations of the sun's corona are described

in detail, then the highly variable non-thermal radio emissions

of centimeter and meter waves. Examples of "synoptic" charts

show sunspot groups, faculae, filaments, eruptions and isophotoes of the "green" corona. A list of publications of regular solar data concludes this useful summary. (Met. Abst.

4.5-248.)-C.E.P.B.

D-54 Beliaev, N. A. , The refraction of extra -terrestrial radio waves

in the atmosphere. (In Russian). Astronomicheskii Zhurnal,

Moscow, 32(4):359-372, July-Aug. 1955. (Transl. by E.R.Hope.

Can. Direc. of Sci. Inf. , Ser. April 1958. 16 p.) -Theoretical

treatment for the case of a quiet undisturbed ionosphere. --Bull.

Sign. Abst.

D-55 Berkner, Lloyd V. (Carnegie Inst, of Wash. ), Signposts to

future ionospheric research. U. S. Air Force. Cambridge Research Center, Geophysical Research Papers, No. 12:13-20,

1952. DWB--A survey of the progress in ionospheric research

beginning with GAUSS a century ago, furthered by discoveries

of MAXWELL and MARCONI and later by CHAPMAN, APPLETON, TUVE and others. The concept of the atmosphere

as a series of heat engines, developed by WULF,

19
is extended to include the F region as a fourth heat engine.

Future efforts should be along the lines of investigating

chemical and photochemical problems, thermo-dynamic processes, atmospheric movements, auroral physics, radio

astronomy, and evolution of the earth's atmosphere (and

consequent evolution of life on earth). (Met. Abst. 4.4-97)

-M.R.

D-56 Berkner, L.V. (Associated Universities, Inc.), The instrumented earth satellite. Science and Culture, Calcutta,

22(10): 553-554, April 1957. DWB, DLC--Seven major ex- periments planned for the U. S. earth satellite are listed and

those plans for radioastronomical observations, micrometeorite and ionospheric studies are explained in more detail.

(Met. Abst. 11J-16.)-M.R.

D-57 Berkner, L.V. (Pres. , Assoc. Universities, Inc., N. Y. ), IRE enters space. Institute of Radio Engineers, N. Y.

,

Proceedings, 47(6): 1048-1052, June 1959. 2 refs. DWB--

Man's escape from the confines of his planet offers him

revolutionary opportunities for performing whole new ranges

of scientific experiments, notably in such fields as astronomy, physics, and geophysics. Electronics, because it

provides the vital nerve system for such experiments, will

be at the very center of these new exploits in space. Moreover, earth satellites, possibly in a 24-hr equatorial orbit,

promise to open a new era in global communications in which

almost limitless bandwidths may become available at relatively low cost. Space will become a major part of the activities of the IRE and its members in the future. Already

there is developing a need for international planning of

space age communications standards and of reguldtions for

utilizing satellites for man's greatest benefit. (Met. Abst.

11.5-181. )--Author's abstract.

D-58 Beynon, W. J. G. and Brown, G. M. (eds. ), Miscellaneous

radio measurements . International Geophysical Year, 1957/

1958, Annals, 3(IGY Instruction Manual): 293-381, 1957.

figs., tables, refs., eqs. Contents: Horner, F. : The mea- surement of atmospheric radio noise, p. 295-314. Morgan,

M. G. : Whistlers and dawn chorus , p. 315-336. Lovell,

A. C. B. ; Forsyth, P. A. and Harang, L. : Radio reflections

from aurorae. p. 337-341. Lovell, A. C.B. : Apparatus for

radio-echo meteor survey, p. 342-345. Bowles, K.L. : Ionospheric forward scatter, p. 346-360. Peterson, A. M. : Ionospheric back scatter, p. 361-381. DWB--This manual gives

a thorough treatment of all aspects of measurement of atmospheric radio noise (theory, equipment, observation methods,

collection of data in centers, etc.), sferics, tweeks, whistlers, the dawn chorus, multiple whistlers, radio reflections

20
from auroras, radio meteor surveys and ionospheric scatter

(forward and backward) for use in IGY program. Samples of

observation forms and records, and elegant photos of equipment are included. (Met. Abst. 9. 9-31. )--M. R.

D-59 Bhonsle, R.V. and Ramanathan, K. R. (both. Physical

Res. Lab. , Ahmedabad), Studies of cosmic radio noise on

25 Mc/s at Ahmedabad. Journal of Scientific and Industrial

Research, Sec. A, New Delhi, 17(12), Special Supplement,

Dec. 1958. p. 40-45. 5 figs. , 4 tables, 6 refs. DWB,

DLC—The results discussed were obtained from March 1957

to Feb. 1958. The method of analysis was to check the

cosmic noise intensity at a local hour, finding the corres- ponding sidereal time, obtaining extra terrestrial intensity

from the (25Mc/s) curve and then calculating the absorption.

The separate contributions of the D and the F2 layers are discussed in relation to the total attenuation. It was found

that D absorption can be <C foF2. Ionospheric irregularities

alone are not responsible for the excess attenuation observed in early night hours. (Met. Abst. 11E-18. )--W. N.

D-60 Bhonsle, R.V. and Ramanathan, K. R. (Physical Res. Lab.,

Ahmedabad, India), Magnetic storms and cosmic radio

noise on 25 Mc/s at Ahmedabad (23"02'N; 72"38'E). Planetary and Space Science, N. Y. , 2(2/3): 99-103, April 1960.

4 figs. , table, 2 refs. DWB--Analyzing the intensities of

cosmic radio noise on 25 Mc/s at Ahmedabad, it was found

that during days of magnetic storms there was, in addition

to the usual variation of intensity due to the diurnal changes

in D region ionization and F region absorption, a further variation. This resulted in a decrease in the attenuation

on the first two days of the storm and an increase in the attenuation on the third day. The decreased attenuation is

most clearly seen in the first half of the night on the first

and second days after the commencement of a storm and is

associated with a decrease in F scatter. (Met. Abst. un- pub.

D-61 Bierman, L. and Lust, R. , Radiation and particle precipi - tation upon the earth from solar flares. Institute of Radio

Engineers, N. Y. , Proceedings, 47(2): 209-210, Feb. 1959.

table, 5 refs. DLC--A brief survey of the main features of

solar emissions in connection with solar flares is given:

ultraviolet and X-ray radiation, corpuscular emission, radio

frequency radiation, and relativistic particles. For these

different components of nonthermal emissions the energies

are estimated and their effects in the ionosphere are briefly

discussed. (Met. Abst. 11. 8-58. ) --Authors' abstract.

21
D-62 Blackband, W.T. (Radio Dept. , Roy. Aircraft Establishment, Farnborough, Hants), Radio communication with a

lunar probe. Royal Society of London, Proceedings, Ser. A,

253(1275):511-515, Dec. 29, 1959. 3 figs. , table, 2 refs.,

eqs. DWB, DLC--In the design of a communication system

between the lunar probe and the earth the study of the radio

noise is of importance. The paper treats the chief sources

of radio noise, the variation of the noise with galactic co- ordinates and the variations of galactic noise with the frequency. A lunar probe might transmit 10 W at a distance

of 400, 000 km. The signal-to-noise ratio could be improved

in three ways: 1) increasing the transmitted power, 2)

using a larger receiving aerial, and 3) stabilizing the axes

of the probe so that a directive transmitting aerial would be

carried with its signal beamed toward the earth. (Met. Abst.

11. 12-483. )»E.K.

D-63 Blackband, W. T. ; Burgess, B. ; Jones, I.L. and Lawson,

G. J. (all, Radio Dept. Royal Aircraft Estab. , Farnborough,

Hants), Deduction of ionospheric electron content from the

Faraday fading of signals from artificial earth satellites.

Nature, London, 183(4669): 1172-1174, April 25, 1959. 2

figs. , table, ref. DWB--There are two classes of fadings

involved: (1) those due to change in energy flux at the re- ceiving aerial and (2) those accompanying a rotation of the

plane of polarization of this energy. The results of a method

used to interpret the fading records of Sputnik I and Sputnik

2 taken at Farnborough and Cambridge show good agreement

of the values of electron content when compared with those

deduced from ionograms taken at Slough and Inverness. The

method of analysis discussed here is reliable. The results are shown in a table and two graphs. (Met. Abst. 11E-22.

)

-W. N.

D-64 Blum, Emile-Jacques; Denies e, Jean-Francois and Steinberg,

Jean-Louis, Etude des orages radioelectrigues solaires de

faible intensite^. (Study of solar radioelectric storms of

weak intensity. ) Academic des Sciences, Paris, Comptes

Rendus, 232(5) :387-389, Jan. 29, 1951. 3 figs. , ref. DWB

--A study of solar radioelectric storms of low intensity which

were observed upon a frequency of 164 Mc/sec has revealed

that days of low activity are characterized by the appearance

of jumps of given amplitude and duration. It is asserted

that intense radioelectric solar storms are produced by the

superposition of jumps. (Met. Abst. 3. 2-197. )--I.L. D.

22
D-65 Blum, E. -J. ; Denisse, J. F. and Steinberg, J. L. , Resultat

des observations d'une eclipse annulaire de soleil effectuees sur 169 Mc/s et 9, 350 Mc/s. (Observational

results of the effects of an annular solar eclipse at the frequencies of 169 Mc/s and 9. 350 Mc/s. ) Annales d' Astrophysique, 15(2):184-198, 1952. 8 figs. , 8 refs. DWB--

The results of observations with 3. 2 and 178 cm wavelength

during the solar eclipse of Sept. 1, 1951 in the French Sudan

are presented and discussed. At 3. 2 cm the distribution of

luminosity increases toward the limb of the disk. At 178 cm

the apparent diameter of the sun by far surpasses the apparent optical diameter, and the distribution of luminosity is

not symmetrical. (Met. Abst. 4. 7-212. )--W. N.

D-66 Blum, E. -J. ; Denisse, J. F. and Steinberg, J. L. , Influence

de l'ionosphere sur la reception du rayonnement qalactique

de frequence 29. 5 Mc/s . (Influence of the ionosphere on

the reception of galactic radiation at frequency 29. 5 Mc/s.

)

Academie des Sciences, Paris, Comptes Rendus, 238(17):

1695-1697, April 26, 1954. 3 figs. , 2 refs. DLC--Observations over 1949-1950 show that galactic radiation on 29. 5

Mc/s is attenuated by the ionosphere. This may be attributed in part to occulation by the F2 layer and in part to supplementary absorption by the D layer. --El. Eng. Absts.

D-67 Boischot, A. and Warwick, J. W. (both. High Altitude Obs.,

Univ. of Colorado), Radio emission following the flare of

Aug. 22, 1958. Journal of Geophysical Research, Wash.

,

D.C., 64(6) :683-684, June 1959. 2 figs. , ref. DWB, DLCAn evaluation of the radio emission on 18 and 40 Mc/s following the flare seen on the Sun on Aug. 22, 1958, is presented from the observations of the High Altitude Observatory, Univ. of Colorado, taking into account the observations on 60 Mc/s from Harvard College Observatory, Fort

Davis, Texas; on 169 Mc/s from Nancy, France; on 470

Mc/s from the National Bureau of Standards, Boulder, Colo. ; and on 2800 Mc/s from Ottawa, Canada. A small flare, importance 1+, was in progress, when the great flare, importance 3 or 3+ , appeared at 1417 UT, and this second flare

was still continuing at 1700 UT. The radio emission showed

an intense outburst, coinciding with the flare as illustrated

on diagrams from 14h 20 m to 16h 20m UT for 18, 40, 60,

169, 470, and 2800 Mc/s, uncorrected for antenna gain.

The complete records on a small time base are corrected for

the effect of lobe, and presented along with ANDERSON's

1958 cosmic ray data. The spectrum differed from that of

typical outbursts observed after great flares, by the great

intensities reached on 40 and 18 Mc/s. Two different types

of emission are indicated: 1) the burst appearing on 2800

and 470 Mc/s with decreasing intensity and frequency

23
disappears near 100 Mc/s; 2) a long enduring continuum

appears later on frequencies lower than 200 Mc/s. The

increase of cosmic rays corresponds better to this second

part of radio emission. The type II emission on metric

wavelengths, which generally immediately follows the

flare, is very weak or non-existent. The probability of a group of type III bursts is suggested. (Met. Abst. 11. 12-

46.)-O.T.

D-68 Bok, Bart J. (Dept. of Astronomy, Harvard Univ. ), New

science of radio astronomy. Scientific Monthly, Wash. , D.C., 80(6): 333-345, June 1955. 5 figs. , 7 photos. DLC--

A nontechnical review of the entire field of radio astronomy

from its first beginnings in 1931 when JANSKY,of Bell Telephone, discovered radio radiation from the Milky Way over

entire range from 1 cm to 30 m, thus extending our tools for

astronomy from a range of 1000 to 30, 000 A (5 octaves) to

12 more octaves of the emission spectrum. Antennas have

grown from 31 ft in 1937 (REBER at Wheaton, 111. ) to 50 ft at N. R. L. in Wash. , D. C. , and 75 ft by Dutch to 250 ft at

Jodrell Bank by Univ. of Manchester, Eng. Effects of sun

on earth's atmosphere are mo/e easily studied by radio frequency radiation variations since they are so sensitive and

extreme in variation. Study of discrete sources, the 21 cm

line of neutral hydrogen and future of radio astronomy in

U.S. are discussed at some length. (Met. Abst. 7.2-76.)

-M.R.

D-69 Booker, Henry G. (Cornell Univ. , Ithaca, N. Y. ), Atmospheric scattering of radio waves, with an application to

radio astronomy (and discussion). U. S. Air Force. Cambridge Research Center, Geophysical Research Papers, No.

11:171-174, 1952. 7 refs. DWB--A theory of atmospheric

scattering (after BOOKER and GORDON, 1950) is applied

to the ionosphere in the hope of explaining "scattering in

the E region, auroral phenomena and scattering in the F re- gion at times of ionospheric storms". The scattering of

radio waves by isotropic turbulence in the ionosphere is

considered. (Met. Abst. 6D-113. )--M. R.

D-70 Booker, H. G. , On the level at which fading is imposed on

waves reflected vertically from the ionosphere. Journal of

Atmospheric and Terrestrial Physics, 7(6):343-344, Dec.

1955. 4 refs. DWB--The observed width of the autocorrelation function at lower frequencies is 6-7 times that given by

theory. Hence, the level of the ionospheric irregularities

causing fading is where the local wave length is 6-7 XA.°,

(Met. Abst. 7. 3-298. )--C.E.P.B.

24
D-71 Booker, H. G. (Cornell Univ. ), Turbulence in the ionos - phere with applications to meteor trails, radio star scintillation, auroral radar echoes, and other phenomena. Journal

of Geophysical Research, Wash., D.C., 61(4):673-705,

Dec. 1956. 11 figs. , 43 refs. , 83 eqs. Also issued in

Journal of Atmospheric and Terrestrial Physics, London,

Special Supplement, Pt. 2, 1957, publ. 1958. p. 52-81.

DLC --Two scales of turbulence are discussed, since large

eddies are responsible for forward scattering phenomena

and small eddies for back scatter. Molecular diffusion

theory forms the basis for small scale eddy formulas; Richardson's number is used for the large scale eddies. Large

eddies have time constants of 40 to 100 seconds; small

eddies about 0. 4 sec near 100 km. Large eddies have a scale of 1.6 km, small eddies about 1.3 meters. The coefficient of eddy diffusion in meteor trails is less than 10 for

small eddies and increases to 10^ for large eddies. The

large eddies responsible for radio star scintillation are located near 200 km. The turbulence power in watt/kg is

given as 5 X 10"'* in the troposphere, 25 at the meteoric

level and 1000 at the scintillation level. (Met. Abst.

10. 8-131. )--S. Fritz

D-72 Booker, H. G. , The use of radio stars to study irregular

refraction of radio waves in the ionosphere. Institute of

Radio Engineers, N. Y. , Proceedings, 46(1): 298-314, Jan.

1958. 19 figs. , 41 refs. , 42 eqs. DLC --Thirteen basic

conclusions are reached after reviewing the observations

and the theory of radio star scintillation. They cover the

methods of observation, observational results, the frequency variation of amplitude scintillations, the diurnal and

seasonal variations of amplitude scintillations, the variation of amplitude scintillations with zenith angle, scintillation rate and phase, the drift of irregularities, the size

of irregularities and the means whereby they are correlated.

(Met. Abst. 11E-26. )-N. N.

D-73 Booker, H. G. (Electrical Eng. , Cornell Univ. , Ithaca, N. Y.)f Phenomena of radio scattering in the ionosphere. (In: American Academy of Arts and Sciences, Atmospheric explorations.

Cambridge, M.I.T. , 1958. p. 101-125. 24 figs. , 35 refs. ) DLC (QC961. A4)--The nature of the ionosphere and VHF ra- dar reflection records is reviewed and illustrated and nine of

the various scattering mechanisms and phenomena explained:

1) fading of quiet echoes; 2) "spread F" phenomenon; 3) as- pect-sensitive echoes; 4) twinkling of point cosmic radio

source noise; 5) long duration meteor trail echoes; 6) echoes from below the E region; 7) VHF scatter communication;

8) echoes from auroral ionization; and 9) "sporadic E" phenomena. Many recorder records, graphs and histograms

25
vividly illustrate the nature of these phenomena. The one

factor which seems to be common to all of these anomalous

conditions in the various ionized media is turbulence, so it is hoped that explanations may be forthcoming in terms of

statistical turbulence theory. (Met. Abst. 11E-25. )--M. R.

D-74 Booker, H. G. (Cornell Univ. , Ithaca, N. Y. ), A local

reduction of F region ionization due to missile transit.

Journal of Geophysical Research, Wash., D.C., 66(4):

1073-1079, April 1961. 6 figs. , 7 refs. DLC- -When Vanguard II was fired from Cape Canaveral, close to 1100 EST,

peculiar echoes were received at intervals between 1102& - 1130 at the monitoring station (approximately 300 km distant) using an ionosphere sounder. The phenomenon is interpreted as produced by the hot exhaust of the passing

missile, and is also discussed in relation to spread F and

radio star scintillations. --W. N.

D-75 Bost, R. (Nat. Lab. of Radio Electricity, Bagneux/Seine),

Influence de 1' eclipse du 30 juin 1954 sur la propagation

des atmospheriques sur la frequence de 27 kc/s. (Influence

of the June 30, 1954 eclipse on the propagation of atmospherics on the 27 kc/s frequency. ) (In: Solar eclipses and

the ionosphere: a symposium. . . ed. by W. J. G. Beynon and

G.M.Brown, London, Pergamon, 1956. p. 132-136. 3 figs.)

DWB--A brief account is given of recordings of atmospherics

on several frequencies during the eclipse of June 30, 1954.

Quite pronounced enhancement was observed for the weaker

atmospherics on 27 kc/s, but no eclipse effects were observed at frequencies in the range 4-12 kc/s. (Met. Abst.

9. 6-289. )--Author's abstract.

D-76 Bowles, Kenneth L. , Incoherent scattering by free electrons as a technique for studying the ionosphere and exosphere: observations and theoretical considerations. U. S.

National Bureau of Standards, NBS Report 6070, Sept. 18,

1959. 39 p. 12 figs., table, 17 refs. , 12 eqs. DWB

(621. 384 U585in). Also issued as: AGARDograph, Paris,

No. 42:223-241, May 1959. 10 figs. , table, 15 refs. -- Incoherent scattering by the free electrons of the ionosphere has been predicted and offered as a technique for measuring the electron density profile both below and above the

F region maximum. This paper reports observations which

confirm the existence of the incoherent scatter and show

that its intensity is essentially the predicted value. The

observed Doppler broadening is considerably smaller than

predicted. In the second part of the paper an explanation

for the reduced Doppler broadening is offered. The scatter

is explained as arising from statistical fluctuations of

26
electron density, the distribution of which is controlled by

the positive ions. Computations of the temporal autocorrelation function, and related power spectrum, of the scatter are presented. An additional possibility of using the

incoherent scatter for mass spectrometer measurements of

the ionic constituents is outlined. (Met. Abst. 11F-13.

)

--Author's abstract.

D-77 Bowman, G. G. (Univ. Queensland, Brisbane), Sunrise and

eclipse effects on the ionosphere at Brisbane. Australian

Journal of Physics, Melbourne, 13(l):52-68, March 1960.

17 figs. , 4 tables, 8 refs. DLC--A rotating spaced-loop

direction finding system, located at Brisbane, has been

operated to investigate sunrise effects by using pulsed 3. 84

Mc/s transmissions, (a) at normal incidence and (b) at oblique incidence. For oblique incidence recording the transmitter was located at Armidale (bearing 202 and distant

355 km from Brisbane). Evidence is presented which suggests the formation (at both E and F2 layer levels) of several frontal irregularities, spaced some tens of kilometers

apart, extending in directions parallel to the sunrise line

and traveling, relative to the earth, with this line. These

fronts pass overhead at Brisbane approximately half way between the 90 km level and ground level sunrise times. In

the post sunrise period, F2 layer spreading on the two hop

trace appears, and the spreading width increases for about

2 hrs, suggesting an F2 layer ripple structure, with increasing ripple amplitude. The post sunrise sporadic E occur- rence suggests frontal irregularities, lying close to the sunrise line direction, soon after sunrise, but indicates a swing

in direction as time progresses. Rotating-loop normal incidence transmissions were also used to investigate effects

due to an eclipse of the Sun, at Brisbane, on April 8, 1959.

Post eclipse E and F2 layer frontal irregularities, oriented

in directions close to the line representing the end of

eclipse in the region of Brisbane suggest a mechanism operating as the eclipse ends, which is similar to that operating

at sunrise. The possibility that the ripple structure which

produces nighttime spread F at Brisbane is generated at sunrise, is discussed. (Met. Abst. 11. 10-142. )--Author"s

abstract.

D-78 Bracewell, Ronald N. and Preston, George W. (both,

Berkeley Astronomical Dept. , Univ. Calif. ), Radio reflection and refraction phenomena in the high solar corona. Astrophysical Journal, Chicago, 123(l):14-29, Jan. 1956.

14 figs. , table, 19 refs. , 13 eqs. DWB, DLC--At the lowest frequencies used in radio astronomy, e. g. , at 18 Mc/s,

the sun has not yet been observed; but if existing data are

correct, it presents a number of curious features: (a) the

27
size of the sun as a radio frequency source is two to three

times the size of the visible sun, but in place of a sharp

limb, there is merely a gradual fading away into the background; (b) a zone of sky is occulted by the sun, and, because significant effects of refraction reach farther out into

the corona than the effects of absorption, the occulted zone

is some nine times larger than the photosphere; (c) the sun

exhibits an occulting disk whose diameter is six times that

of the photosphere and which differs from the emitting disk

in having a sharp limb; (d) the discrepancy in size between

the occulted zone and the occulting disk is associated with

apparent displacement of the unocculted sky toward the sun

by refraction; (e) within the occulting disk the sun behaves

as a convex reflector, mirroring the whole of the unocculted

sky. The reflection of the Galaxy, though greatly diminished in size, remains comparable as a radio source with

the emitting sun itself. If observed with existing aerials,

which are incapable of resolving the solar emission from

the galactic reflection, the sun should apparently exhibit

a marked annual variation of flux density. (Met. Abst.

9A-106.) -Authors' abstract.

D-79 Bracewell, R. N. , Radio interferometry of discrete sources . Institute of Radio Engineers, N. Y. , Proceedings, 46(1):97-

105, Jan. 1958. 4 figs. , 13refs., eqs. DLC- -Salient features of the theory and practice of radio interferometry are presented with special attention to assumptions and to the

specifically two-dimensional aspects of the subject. The

measurable quantity on an interferometer record is defined

as complex visibility by generalization from an analogous

quantity in optical interferometry. Subject to conditions on

antenna size and symmetry, the observed complex visibility

is equal to the normalized two-dimensional Fourier transform

of the source distribution, with respect to certain variables,

Sx and Sy, which are defined. This transform is in turn

identically equal to the complex degree of coherence T between the field phasors at the points occupied by the interferometer elements. The correlation between the instantaneous fields, and that between the instantaneous intensities are less general parameters which are, however, deducible

from 1 . A theorem is proved according to which only cer- tain discrete stations on a rectangular lattice need be occupied for full determination of a discrete source distribution.

Procedures in interferometry are discussed in the light of

this result and an optimum procedure is deduced. Current

practice is considered overly conservative, e. g., independent data in the case of the sun are obtainable only at station

spacings of about 100 wavelengths on the ground, a fact

which hitherto has not been taken into account. (Met. Abst.

unpub. )--Author's abstract.

28
D-80 Bracewell, R.N. and Stableford, C.V., Critical frequency,

refractive index, and cone of escape in the solar corona . Institute of Radio Engineers, N. Y. , Proceedings, 46(1):

198-199, Jan. 1958. fig. , 4 refs. DLC--Since propagation

and escape of radio waves in the solar corona have much in

common with propagation in the ionosphere, the nomograms

presented are offered to facilitate the calculations of numerical results. --W. N.

D-81 Bracewell, R. N. and Garriott, O. K. (both, Radio Propagation Lab. , Stanford, Univ. Calif. ), Rotation of artificial

earth satellites. Nature, London, 182(4638): 760-762, Sept.

20, 1958. 7 figs., 3 refs. , eqs. DLC -The influence of

rotation of an artificial satellite on its earth bound radio

signal is discussed. Representative examples of regular

fading of the 20 and 40 Mc/s signals from Sputnik I, as re- corded when the satellite passed Stanford, are given along

with a brief theoretical discussion on elimination of rotational effects. Features of the field strength of Sputnik III,

of June 14, 1958, indicate that the problem was then solved.

(Met. Abst. unpub. )--W. N.

D-82 Bracewell, R. N. (Radioscience Lab. , Stanford Univ. ), Communications from superior galactic communities . Nature,

London, 186(4726) :670-671, May 28, 1960. fig. , 6 refs.

DWB--DRAKE (1959) has described equipment under construction to look for transmissions from advanced societies

elsewhere in the Galaxy. He plans to look at Ceti and Eridani. It seems more reasonable that we look for probes

sent here, and we in turn send probes. The important thing

for us is to be alert to the possible interstellar origin of un- expected signals and be prepared to communicate with the

sender. (Met. Abst. 11. 12-491. )--E.Z. S.

D-83 Bracewell, R. N. , Correcting noise maps for beamwidth. (In: Menzel, Donald H. , ed. , The radio noise spectrum.

Cambridge, Mass. , Harvard Univ. Press, 1960. p. 141-150.

5 refs., eqs. DWB-Two kinds of practical problems arise

in correcting noise maps for beamwidth which are referred to

as "smoothing" and "sharpening. " The first of these arises

when we have a detailed survey available and wish to find

what we would observe with a beam wider than that used for

the survey. The second comes up when we are given the

data from a survey made with an antenna having a known

radiation pattern and we wish to ascertain what would have

been observed had we used an antenna with a narrower beam.

We consider first the discrete interval theorem which is valuable for the handling of two-dimensional data since it en- ables numerical work to be done at rather coarse discrete

intervals without loss of accuracy. One section of this

29
paper is devoted to exploration of the procedure for smoothing survey data to yield values appropriate to broader circular asymmetric beams. Practical numerical details are dealt with in a section on adjustment of scale factors and

finally the sharpening procedure is discussed. (Met. Abst.

unpub. )--E. Z. S.

D-84 Bremmer, H. , Exploring the atmosphere with radio waves.

Philips Technical Review, 22(3):61-70# Jan. 14, 1960.

2 figs. , 29 refs. DLC--This is a compressed version of the

author's inaugural address as extramural professor at the

Eindhoven Technische Hogeschool, Feb. 12, 1960. The

general review of scientific accomplishments is discussed

in terms of the ionosphere as a hypothesis to explain the

range of radio waves, sounding in the ionosphere, the

space above 400 km, transition of the atmosphere to interplanetary gas, ionospheric winds, radar observation of

meteors, and atmospheric tides. --W. N.

D-85 Brenan, I. N„ (Nuffield Radio Astronomy Lab. , Univ. of

Manchester), The correlation of radio source scintillation

in the Southern and Northern Hemispheres. Journal of Atmospheric and Terrestrial Physics, London, 19(3/4): 287-289,

Dec. 1960. fig. , table, 10 refs. DWB--This research note

presents the results of a comparison of scintillation observations made during the IGY at the Royal Society Base,

Halley Bay, Antarctica, and the simultaneous observations

made at Jodrell Bank in England. The positions of the stations and their coordinates are given in tabular form. The

comparison was made in order to determine whether or not

the scintillation activity in high southern latitudes is re- lated to the activity in northern latitudes, and the results,

graphically presented, show the correlation coefficient as

+ 0.37 for 388 pairs of observations. This coefficient is

compared with other values published on the day to day cor- relation of scintillation activity and the resulting theoretical

implications are discussed. (Met. Abst. unpub. )--I. S.

D-86 Brenan, P.M. (Jodrell Bank Experimental Station, Univ. of

Manchester), Ionospheric drifts determined from radio-star

scintillation observations. Royal Society of London, Proceedings, Ser. A, 256(1285): 222-229, June 21, 1960. 5

figs. , 8 refs. DLC- -Spaced receiver observations of radio

star scintillation were made at the Royal Society Base,

Halley Bay, during the I. G. Y. A technique is described

whereby ionospheric velocities can be deduced from the

motion of the diffraction pattern on the ground. These velocities were approximately toward the west in the first part

of the night, and toward the east for the rest of the night

and most of the next day. The reversals in direction of

30
motion occurred at 0030 and 1630 L.M.T. Lift speeds were

of the order of 400 m/s in the evening, falling to 100 m/s

after easterly motions had been established. Both the time

of midnight reversal and the drift speed correlate well with

Evan's (1959) measurements of motions of auroral forms.

(Met. Abst. unpub.

)

D-87 Briggs, B. H. (Cavendish Lab. , Cambridge), Diurnal and

seasonal variations of spread-F ionospheric echoes and the

scintillations of a radio star. Journal of Atmospheric and

Terrestrial Physics, London, 12(2/3) :89-99, 1958. 7 figs.

,

table, 12 refs. DLC--A comparison is made of the spread F

ionospheric echoes observed at Slough (52 N) and Inverness

(57 N). It is found that the degree of spreading is greater

at the station of higher latitude. The diurnal and seasonal

variations are similar at the two stations. The diurnal and

seasonal variations of the scintillation index of the radio

star in Cassiopeia are explained in terms of measured ionospheric parameters (spread-F index and critical frequency)

together with the change of zenith angle of the source. A

large seasonal anomaly, which was previously thought to

exist, is found to be much reduced when all the relevant

factors are taken into account. (Met. Abst. 10. 2-168. )--

Author's abstract.

D-88 Briggs, B. H. (Cavendish Lab. , Cambridge), A study of the

ionospheric irregularities which cause spread-F echoes and

scintillations of radio stars. Journal of Atmospheric and

Terrestrial Physics, London, 12(l):34-45, 1958. 5 figs.

,

4 tables, 22 refs. DLC--A study is made of the correlation

between the occurrence of spread F echoes at Slough, Inverness and Oslo. It is concluded that the ionospheric irregularities which cause the spreading occur in patches which

have dimensions of the order of 500 km in a NS direction,

and considerably greater in the EW direction. There is an

indication that these "bands" of irregularities may lie along

lines of magnetic latitude, and the fact that they tend to

occur in the same geographical position on successive nights

at two places is investigated. The results are found to be

consistent with the same picture of the spatial distribution

of the irregularities causing the scintillations which are at

heights near 300 km. (Met. Abst. 9. 11-163. )--Author's

abstract.

D-89 Brito-Infante, Jose M. (Escuela de Electronica, Armada de

Chile, Vina del Mar, Chile), Elimination of ionospheric

refraction effects . Institute of Radio Engineers, N. Y.

,

Proceedings, 49(9): 1451 -1452, Sept. 1961. table, ref.

,

6 eqs. DLC --Describes a simple method of eliminating

ionospheric refraction effects upon signals emitted from

31
a mobile high altitude radio transmitter. By this method,

an orbiting satellite can, in effect, be located by direct

analysis of the Doppler effect of the satellite transmitted

radio signals as demonstrated. (Met. Abst. unpub. )--W. N.

D-90 Brockman, M.H. ; Buchanan, H. R. ; Choate, R.L. et al.

,

Extraterrestrial radio tracking and communication. Institute

of Radio Engineers, N. Y. , Proceedings, 48(4): 643-654,

April 1960. 10 figs. , 5 tables, 11 refs. , numerous eqs.

DLC--When the U. S. Army lunar program was initiated in

1958, the Jet Propulsion Laboratory (JPL) was assigned the

responsibility for the upper rocket stages and the payload.

Payload responsibility included radio tracking and communication with the lunar probe. JPL's Microlock system, used

for communicating with the early Explorer satellites, did

not have sufficient range to perform this mission. Therefore, a new radio system designated TRACE (E) (Tracking

and Communication, Extraterrestrial) was designed. To the

best knowledge of the authors, the TRACE (E) system is the

first deep space communication link to provide accurate

tracking and telemetry data at lunar distances. The design

principles of the TRACE (E) system are presented in this

paper in conjunction with a description of the equipment

and actual performance data taken during the Pioneer IV

lunar mission in March 1959. The TRACE (E) system is an

integral part of the NASA/JPL radio tracking station located

near Goldstone Lake north of Barstow, Calif. Future plans

for improving the performance of the TRACE (E) system are indicated. (Met. Abst. 11. 10-40. )--Authors' abstract.

D-91 Brockman, James (Nat. Bur. of Standards. , Boulder Lab. , Colo. ), Solar disturbances and radio communication fore - casts . Sky and Telescope, 21(6): 322-326, June 1961. 9

figs. DLC--An account of the 3+ solar flare of Nov. 12,

1960, which disrupted the atmosphere and the earth's magnetic field for almost 10 days. Illustrative of the present

day forecast service is how the forecaster J. Weldon, at

the World Warning Agency at Fort Belvoir, Va. , reacted

after being taken by surprise and immediately transmitted

his successful forecasts. --W. N.

D-92 Brown, Robert Hanbury and Lovell, A. C.B. , Exploration of

space by radio. N. Y. , John Wiley, 1958. 207 p. 132 figa

(incl. photos), 6 tables, bibliogs. DLC (QB475. B7. Review by T. Krishnan in Journal of Scientific Research, New

Delhi, Ser. A, 18(3): 141-142, March 1959. -A new, semitechnical textbook on the astronomical, theoretical, instrumental, observational and specialized aspects of radio

astronomy, nicely illustrated with photographs of radio

telescopes, equipment, instruments, records, graphs, etc.

32
Separate chapters are devoted to the galactic and extragalactic radio emissions, the hydrogen line, scintillation

of radio stars, solar radio emissions, meteors, radio and

the aurora, the moon, planets, earth satellite, and finally, a description of the Jodrell Bank radio telescope and the

program of research. Techniques are thoroughly discussed

in Ch. 3, and ionospheric-geomagnetic effects on radio

emissions from space in Ch. S. The chapter on radio observations of the aurora is especially complete. (Met.

Abst. 10.7-9.)--M.R.

D-93 Brown, R.H. and Hazard, C. (both, Nuffield Radio Astronomy Labs. , Jodrell Bank), Radio emission from normal

galaxies, Pt. 2. A study of 20 spirals at 158 Mc/s. Royal

Astronomical Society, London, Monthly Notices, 122(8) :479-

490, 1961. 3 figs., 3 tables, 9 refs. , 5 eqs. DLC -A sur- vey has been made of the radio emission at 158 Mc/s from

20 bright spiral galaxies. A radio index R has been defined

by the equation R = m — m , where m and m are the

r pg' r pg

radio and photographic magnitude respectively. The results

indicate that R is a function of the inclination and galactic

latitude of a galaxy and it is suggested that this effect is

due to the absorption of light. The mean value of R for

spirals of type Sb and Sc is + 1. 3 with an r. m. s. dispersion + 0. 7. No significant difference was found between

the mean values of R for the two types of galaxies. (Met.

Abst. unpub. ) --Authors' abstract.

D-94 Brown, S. B. and Petrie, W. , The effect of sunrise on the

reflection height of low frequency waves. Canadian Journal

of Physics, 32(l):90-98, Jan. 1954. fig. , 3 tables, 12 refs.,

23 eqs. DLC--The observed sudden changes of phase and

amplitude of 16 kc/s waves transmitted over distances of

540 km are discussed in relation to the geometry of the system at the change-over from night time to day time reflection

height (95 km and 70 km respectively). The effect cannot

be due to photoionization of atmospheric molecules, but may

be due to removal of electrons from negative oxygen ions by

visible and near infrared radiations; calculations are presented giving support to this view. The rate of fall of the

reflection height is discussed. --IRE Abst. 2092.

D-95 Bruce, G.E. R. (Electrical Research Association Lab.

,

Leatherhead, Surrey), The energy radiated by radio galaxies . Institution of Electrical Engineers, Journal, 7(80):513, Aug.

1961. 3 refs. DLC --The electric field and discharge theory

explain the amount, as well as how the energy radiated by

radio galaxies transform globular or elliptical galaxies into

irregular or spiral ones, as suggested by the author in 1944.

Consultation of available literature is advisable prior to

postulations. --W. N.

33
D-96 Bruzek, A. (Fraunhofer Institut, Freiburg i. Br. ) f Die

Radiowellenstrahlung der Sonne, II, Per m-Wellenlangenbereich. (Radio wave radiation of the sun, Pt. 2, The

meter wave region. ) Umschau, Frankfurt a. M. , 22(50):

684-686, Nov. 1959. 5 figs. , 2 foot-refs. , 8 refs. DLC--

Studies of the long lived radio wave radiation have shown

that the intensity of the "quiet" meter wave radiation and

its distribution over the solar disk varies from day to day.

In the meter region there exists also local centers of intensified quiet radiation. Its effective radiation of about

g

2 x 10 degrees indicates a thermal origin. The radio

storms constitute another long level but restless radiation.

The meter wave bursts consist of five types. Type I bursts

have a life several tenths of a second to one second; a band width of 4 to 7 MHz and they do not change their frequency. The type III bursts have a similarly brief duration

but at a band width of 10 MHz, they manifest a rapid frequency drift of about 20 MHz/sec. Type II bursts are powerful radiation outbursts with apparent temperatures of

11 14 10 ' to 10 degrees which often extend over the spectral

region of 8. 5 to 33 met. The type IV bursts consist of a rapid rise in radiation intensity with circularly polarized

radiation following a type II burst. (Met. Abst. 11. 9-110. ) --I.L.D.

D-97 Budden, K:C. and Ratcliffe, LA. (Cavendish Lab. , Cambridge, England), An effect of catastrophic ionospheric

disturbances on low-frequency radio waves. Nature, London,

140(3555): 1060-1061, Dec. 18, 1937. 2 figs. , 3refs.DLC

--Recordings of long standing of the down-coming wave at

16 kc/s were analyzed and compared in relation to time of

fadeouts, increases in spherics and magnetic anomalies on

the same day. The results presented in curves show a marked effect of LF waves at the 70 km level. --W. N.

D-98 Budden, K. G. and Yates, G. G. , A search for radio echoes

of long delay. Journal of Atmospheric and Terrestrial Physics, 2(5):272-281, 1952. 23 refs. DWB--An unsuccessful

search was made for echoes delayed 3-15 sec. The cause

of such echoes is discussed and they are tentatively attributed to "the propagation of guided waves over long curved

paths formed by belts of ions outside the earth but fixed

relative to it." (Met. Abst. 4. 4-100. )--C.E.P.B.

D-99 Bugnolo, Dimitri S. , Radio star scintillation and multiple

scattering in the ionosphere. Institute of Radio Engineers,

New York, Transactions, Vol. AP-9(l):89-96, Jan. 1961.

8 figs. , 10 refs. , 46 eqs. DLC--

34
The transport equation for the expectation of the photon

density function, as applied to multiple scattering in the

ionosphere, is used here to predict the mean squared scattering angle and corresponding size of the ionospheric ir- regularities as measured on earth. The results derived,

based on a Gallet model for turbulence in the underside of

the F layer at night time conditions, are applicable to other

models as well. --From Author's abstract.

D-100 Bureau, R. , Effect of catastrophic ionospheric disturbances

on low- frequency radio waves. Nature, London, 141(3571):

646, April 9, 1938. fig. --Very brief note on observations

at 12, 17, 22, 27 and 30 kc/s at Paris, St. Cyr, and Rabat,

France, on Nov. 6, 1936, confirming Budden and Ratcliff's

results. (See ref. D-97.)

D-101 Burgess, R.E. and Fowler, C.S. , Solar activity and ionospheric effects. Comparison from May to Nov. 1948. Wireless Engineer, London, 29(341) :46-50, Feb. 1952. 4 figs.

,

table, 3 refs. DLC- -Observations of ionospheric propagation

conditions on long waves (191 kc/s) and short waves (18. 89

Mc/s) were compared with observations of solar noise bursts

(on 30, 42, 73 and 155 Mc/s) and with the appearance of

solar flares and sunspots. Detailed study of the correlation between these phenomena was made and statistical conclusions are presented. (Met. Abst. 6D-116. )--M.L. R.

D-102 Burkard, O. (Inst, for Met. and Geophysics, GrazUniv. ), Radio reflexions from the moon and solar corona . Nature,

London, 183(4669): 1180, April 25, 1959. 5 refs. , 3 eqs.

DWB--A revised formula for the plane of polarization which

is based upon the assumption that there are some hundred

electrons per c. c. in the space around the earth is given

here. The "old* formula for the rotation of the plane of polarization is also given in this brief discussion. The modification is based on Sputnik I researches. (Met. Abst. 11.

10-97. )-W. N.

D-103 Burrows, Charles R. (Dir. School Elec. Engr. , Cornell

Univ. ), Radio astronomy. Electronics, Albany, N. Y.

,

22(2):75-79, Feb. 1949. 5 figs. , 13 refs. DWB. Also in:

Cornell Univ. School of Electrical Engineering, Contract

N6onr-264, T. O. 6, NR077-321, Radio 'Astronomy Report

No. 3, Feb. 1949. (5 p. ) 5 figs. , 13 refs. DWB--A broad

informative presentation of the subject and its various as- pects with the focus on radio astronomy as a useful tool for

the radio engineer, the astronomer and the meteorologist.

(Met. Abst. 9A-7. )-W. N.

35
D-104 Cain, J. C. ; Shapiro, I. R. ; Stolarik, J. D. and Heppner,

J. P. (all, Space Sci. Div. , Goddard Space Flight Center,

NASA, Greenbelt, Md. ), A note on whistlers observed

above the ionosphere. Journal of Geophysical Research,

66(9): 2677-2680, Sept. 1961. 4 figs. , 11 refs. DLC--The

sensing coil of the proton precession magnetometer carried

on the Vanguard III satellite, also served as an antenna for

detecting audio frequency electromagnetic waves. A preliminary analysis is given for about 100 whistlers observed

Sept. 18 through Dec. 12, 1959, at low altitudes over the

altitude range 510 to 3750 km. About 90% of the whistler

occurrences are between 6 P. M. and 6 A. M. local time,

indicating a low nighttime absorption by the ionosphere.

The intensity of the H component of the wave is estimated

to be between 0. 01 and 0. 5 gamma, with that of a few signals exceeding 1 gamma. --Authors' abstract.

D-105 Carnegie Institution of Washington, Yearbook, No. 54.

July 1. 1954/June 30. 1955. Wash., D.C., 1955. 311 p.

figs. , tables, bibliogs. DWB--Reports of departmental

activities and cooperative studies: Mount Wilson and Palomar Observatories, p. 3-38, 3 tables, bibliog. , p. 36-38.

Department of Terrestrial Magnetism, p. 41-94, 17 tables,

bibliog. p. 91-94. Solar research (photography, sunspot

and magnetic studies, and solar spectrum investigations)

at Mount Wilson and other observatories is outlined. Work

in radio astronomy of Jupiter, the sun, and galaxies and

ionospheric effects on radio frequency radiation is described. Cosmic ray investigations (by S. E. Forbush) are summarized. (Met. Abst. 8. 1-37. )--M. R.

D-106 Carnegie Institution of Washington, Yearbook. No. 56.

July 1. 1956-June 30. 1957. Wash., D.C., 1957. 425 p.

figs. , tables, bibliogs. Reports of departments and special

studies: p. 37-75, Mount Wilson and Palomar Observatories,

p. 81-87, Dept. of Terrestrial Magnetism, p. 149-252, Geophysical Laboratory. DWB--The report on the Mt. Wilson

and Palomar Observatories describes the work in progress

and some of the results of solar research (solar photography,

sunspot activities, solar magnetic fields, geomagnetic relations, radio sources, etc. ). The report of the Department

of Terrestrial Magnetism goes into radio astronomy research — radio emissions from the sun, Jupiter and Venus, upper

air winds and radio star scintillations, etc. The IGY program is outlined. Extensive bibliographies accompany each

report. (Met. Abst. 10. 5-23. )--M. R.

36
D-107 Carpenter, Martha (Stahr), Bibliography of radio astronomy. Cornell Univ. School of Electrical Engineering, Contract

NSonr-26406, Radio Astronomy Report No. 2, Dec. 15,

1948. 44 p. Also First Supplement, issued as Radio Astronomy Report No. 4, July 1, 1949. 25 p. And Second

Supplement, issued as Radio Astronomy Report No. 10,

Feb. 15, 1950. 25 p. --The first issue contains 117 references, mostly annotated, and pertaining wholly or in part

to that phase of radio astronomy which deals with radio

frequency radiations from extraterrestrial sources. The

references are arranged chronologically and then alphabetically by authors within the following 6 sections: 1. Observations of galactic noise; 2. Observations of solar

noise; 3. Theory of emission of radio waves by the galaxy;

4. Theory of the emission of radio waves by the sun; 5.

Theory and description of instruments; and 6. Reviews.

The first supplement includes a total of 67 references numbered consecutively to the former bibliography. The second

supplement contains 51 references, follows the same ar- rangement as previously but includes an additional section

on observations of radio frequency radiation from the moon.

-W. N.

D-108 Carpenter, Martha (Stahr), Bibliography of extraterrestrial

radio noise. Issued as part of the Report of Commission V

to the 9th General Assembly of the International Scientific

Radio Union. Cornell Univ. School of Electrical Engineering, Contract N6onr-2S406, Radio Astronomy Report No. 11,

Aug. 15, 1950. 129 p. 280 refs. Also Supplement for

1950, issued as Part of the Report of Commission V to the

10th General Assembly of the International Scientific Radio

Union. Pub. as Radio Astronomy Report No. 12, Aug. 1952.

63 p. "77 items which appeared in 1950. "--The annotated

references are classified according to: (A) Radiation from

the sun; (B) General galactic radiation; (C) Radiation from

""discrete sources"; (D) Radiation from the moon. In each

section the works are divided into (1) observations, and

(2) theories and interpretations, and chronologically within

each subsection. Also a section on miscellaneous items

and one on reviews are included. Many of the abstracts

are from standard journals and about half by the author. An

author index is appended. Titles are given in the original

language (except Russian titles which are given only in

English translation).

Note: A bibliographic reference mentions that Radio Astronomy Report No. 13 brought the bibliography up to date

through 1951. Also Supplement for 1952. Issued as Cornell

Univ. School of Electrical Engineering, Contract Nonr-40122,

Research Report EE371, April 15, 1958. 1 vol. incl. tables.

Available from ASTIA as its AD-204-812. (UNCHECKED).

37
Note: In 1957, the Australia Commonwealth Scientific and

Industrial Research Organization. , Div. of Radiophysics,

brought out its Radio Astronomy bibliography, 1954-1956,

as a "tentative bridging of the gap between existing and

projected publications of the Cornell Univ. Bibliography of

extraterrestrial radio noise." --M. ft- and D- fi.

D-109 Carru, H. ; Gendrin, R. and Reyssat, M. (all. Centre

National d'Etude de Telecommunications, Departement Communications et Detection Spatiales, Issy-les-Moulineaux),

A transatlantic communication via Echo I satellite. Nature,

London, 189(4761): 268-271, Jan. 28, 1961. 5 figs. , 5 refs.

DWB--This paper describes in detail a successful experiment involving communication, using continuous wave transmissions between Holmdel (New Jersey) and Issy-les-Molineaux (France) which took place on Aug. 18, 1960. The fact

that this was the only successful attempt in 12 trials may

have been due to a lack of the necessary signal strength.

The signal in this case was received for about 1 min. The

amplitude trace is illustrated. In order to make some comparison with the theoretical prediction the position, distance and Doppler effect for the time were computed. From

the Doppler curves the transmitted frequencies are estimated

Examination of the amplitude record showed that the reflectivity to the coating is almost ideal and that the received

signals are free from rapid fading. (Met. Abst. unpub.

)

--R. B.

D-110 Chapman, J. H. and Molozzi, A. R. (Defence Res. Telecom.

Estab. , Ottawa, Canada), Interpretation of cosmic noise

measurements at 3. 8 Mc/s from satellite 1960 %/ 1. Nature,

London, 191(4787) :480, July 29, 1961. table, 2 refs. DLC

--Tentative analysis of the field strength variations according to locations were made. The brief discussion is based

on the following assumptions as causes of the variation:

(1) variation of the antenna's radiation resistance; (2) re- striction in angular aperture of the antenna; and (3) variation of cosmic noise power over the sky. Very brief tabulated results are given since a detailed report is to be published. -W. N.

D-lll Chapman, Sydney, The sun, the earth's atmosphere, and

radio transmission . Nature, London, 1 19(2994) :428-429,

March 19, 1927. --A general informative article on propagation of radio waves through the atmosphere and the effect

of solar activity directly responsible for the variable conditions of radio communication. --W. N.

38
D-112 Chapman, S. and Little, C. Gordon, The nondeviative

absorption of high frequency radio waves in auroral latitudes. Journal of Atmospheric and Terrestrial Physics,

10(1):20-31, Jan. 1957. 3 tables, 21 refs. , 14 eqs. DWB

--In auroral latitudes the nondeviative absorption of high

frequency radio waves is much more irregular, and often

much stronger, than in subauroral latitudes. It is greater

and more frequent by day than by night; this is the converse of the daily variation of magnetic activity. The electrons that produce the absorption in subauroral latitudes are mainly caused by solar ultraviolet light; in auroral

latitudes, often the major source is bombardment of the

atmosphere by solar gas. According to J. A. VAN ALLEN's

new interpretation of the soft radiation observed by himself and his colleagues in auroral latitudes, down to 50 km,

a small minority of the primary bombarding particles generate X-rays, which penetrate further than the particles

themselves. It is here suggested that the layer ionized

by these X-rays is an important factor in the daytime radio

absorption. Also, as D.R.BATES has pointed out, Lymanalpha radiation will be generated by the auroral protons;

ionization of nitric oxide molecules by this radiation may

also contribute appreciably to the absorption. The same

processes of ionization will occur likewise at night, .and

often still more strongly; however, loss of the electrons

to form negative ions by attachment is countered by photodetachment during the day, but not at night. Very tentative tables are given, based on these ideas, indicating

ionospheric conditions consistent with greater daytime absorption than at night, even when the nighttime bombardment is twenty times more intense than that by day. The

corresponding absorption relaxation times, and daily variation of magnetic disturbance, will be examined in a later

note. (Met. Abst. 8. 6-179. )--Authors' abstract.

C-113 Chapman, S. , The earth in the sun's atmosphere. Scientific American, N. Y. , 201(4) :64-71, Oct. 1959. 10 figs,

(incl. photos). DWB, DLC--The magnitude of our Earth and

the extent of its surrounding atmosphere as well as the density of the solar atmosphere is discussed. Although a knowledge of the physical Earth and of the astronomical

science associated with the earth dates back over 2000

years, little was known of the significance of the conductivity that exists between the earth's and the sun's atmosphere, their electron densities, and of the violent prominences in the photosphere that emit energy which, in turn,

is carried away by convection within the solar atmosphere.

The present report covers the achievements made along

these lines during the IGY. It describes numerically the

density and intensity of the electrons in the solar

39
atmosphere, turbulent waves and temperature rises within

the solar region. Close to our earth it is recorded that

over S000 electrons, and the same number of protons, per

cu in. exist. This means that in the interstellar space

these figures range from 10 to 200 per cu in. The article

indicates that the hot energizing solar gas steadily streams

into our earth's atmosphere and the deflected particles of

such gases give birth to the observed luminous aurora. Some of it is trapped in the outer belts of the atmosphere.

Photographs of the corona, the zodiacal light, etc. , as

well as graphical illustrations of the earth's temperatures

in degrees Kelvin, the electron densities per cu in. and

the reflection of radio waves from the ionosphere as re- corded in the Propagation Laboratory in Boulder, Colo., are included. (Met. Abst. 11. 9-73. )--N. N.

D-114 Chechik, P. O. , Radiotekhnika i elektronika v astronomii.

(Radiotechnique and electronics in astronomy. ) Moscow,

Gosenergoizdat, 1953. 103 p. 76 figs. , 22 tables, footrefs. , bibliog. (38refs.) p. 102-103. Massovaia Radiobiblioteka, No. 189. DLC (QB475. C45) -This small technical text contains chapters on various aspects of time (or

longitude) on earth and its radio dissemination or determination; on meteors and their study by radio; on lunar, solar

and galactic investigations by radio, on the significance

and application of photo-elements in astronomy and their

measurement. The effect of the ionosphere, ionospheric

winds, solar influences in magnetic field of earth and radio

frequency radiation from sun and space are all treated. All

references are to Soviet literature. (Met. Abst. 8H-28. ) --M.R.

D-115 Chestnov, F. I. , Zagadka ionosfery. (Enigma of the ionosphere.) Moscow, Gosud. Izdat. Tekhniko-Teoreticheskio

Literary, 1954. 54 p. 24 figs. Nauchno-populiarnaia

Biblioteka, No. 70. DLC --The detailed structure of the ionosphere is described and shown in an original schematic

diagram. Ionization, twilight, night sky light, aurora, diurnal effects, magnetic field, magnetic storms in ionosphere, solar effects, radio propagation (long and short

wave), ionospheric soundings by radio impulses, sunspot

effects, forecasts of radio propagation, meteor traces, ra- dio radiation from stars and rocket exploration of ionosphere are treated in condensed popular technical form.

(Met. Abst. 6D-235. )-M.R.

40
D-116 Child, C.H. (North American Aviation, Inc., Downey,

Calif. ), Requirements for data transmission from a Martian

Reconnaissance Vehicle. Advances in the Astronautical

Sciences, New York, Vol. 5, 1959, issued 1960. p. 261-

277. 12 figs., table, 10 refs. , 4 eqs. DWB (629.1388

A512pro), DLC (QB1. A26)--An analysis is presented of

the requirements for a communication system on a Solar

System Reconnaissance Vehicle. The effects of various

noise sources are evaluated in terms of their influence on

operating frequencies. Transmitter power levels, receiver

sensitivity, and noise figure properties are discussed in

terms of present and projected developments. An operating frequency of approximately 850 Mc is recommended on

the basis of maximum anticipated advances in the state of

the art during the next 3 to 5 years. In terms of these advances, it appears that a transmitter power supply weight

of approximately 300 lbs will be required to produce an rf

power output of approximately 10 kw. Lesser degrees of

advancement would cause the weight to increase to approximately 500 lb and the required power output to increase to

approximately 60 kw. The problem of heat dissipation,

based upon 50% conversion efficiency, is left to the airframe structures and thermodynamics groups. (Met. Abst.

11. 12-481.) -Author's abstract.

D-117 Chivers, H. J. A. and Greenhow, J. S. (both, Univ. of

Manchester, Jodrell Bank Experimental Station), Auroral

ionization and the absorption and scintillation of radio

stars. Journal of Atmospheric and Terrestrial Physics,

N.Y. , 17(1/2):1-12, Dec. 1959. 6 figs. , 15 refs. DWB,

DLC --The absorption of the radiation from extraterrestrial

radio sources, when observed at low elevations to the

north of Jodrell Bank (geomag. lat 56 ), is discussed. At

lower culmination the Cygnus radio source is at an elevation of only 4 , and the line of sight to the source then

passes through the ionosphere near the zone of maximum

auroral activity. Combined observations of the source intensity at 36 Mc/s and 100 Mc/s, and of radar back-scatter

echoes at 38 Mc/s, have been made using the 250 ft steerable telescope. The absorption and certain back-scatter

echoes can be related to an ionized layer at a height of the

order of 100 km, associated with auroral activity. It is

shown that with a high sensitivity radar equipment at 36

Mc/s, weak auroral type echoes from irregularities in the

E region aligned along the earth's field occur on about 40%

of all days at quite low geomagnetic latitudes. The suggestion is made that the scintillation of radio stars observed from latitudes similar to that of Jodrell Bank is not due

entirely to irregularities in the F region, but that there is a large contribution from these aligned irregularities at E re- gion heights. (Met. Abst. 11. 7-163. ) --Authors' abstract.

41
D-118 Chivers, H.J. A. and Wells, H. W. (both, Jodrell Bank

Experimental Station, Manchester Univ. ), A new ionospheric phenomenon. Nature, London, 183(4669): 1178,

April 25, 1959. fig. , 5 refs. DWB--In order to eliminate

man-made noise and interferences, a special study of some

unusual radiations began at Jodrell Bank in Oct. 1958. Five

separate total power receivers, slightly differing, but near

80 Mc/s were used; three receivers were at Jodrell Bank,

the other two at separate sites at 1 km distance. Some ten

instances of isolated increase of the noise level were re- corded by some of the instruments while others simultaneously recorded decrease during the period Jan. 3-10, 1959.

Again, on March 25, 1959, at 1400 U.T. a very striking

isolated event occurred. Facsimile recordings are given.

Preliminary investigations of these rare, seemingly precur

sors of stepped-up solar activity and subsequent magnetic

storms and auroras, show no unusual solar or terrestrial

effect or relationships. (Met. Abst. 11F-21. )-W. N.

D-119 Chivers, H. J. A. (Univ. of Manchester, Jodrell Bank Exper.

Sta. ) and Wells, H. W. (Carnegie Inst. , Wash.), Observations of unusual radio frequency noise emission and absorption at 80 Mc/s. Journal of Atmospheric and Terrestrial Physics, N.Y. , 17(1/2): 13-19, Dec. 1959. 2 figs.

2 tables, 11 refs. DWB, DLC --Unusual radio frequency

noise emissions at 80 Mc/s have been identified during

periods of solar activity. The noise enhancements may be

classified as (1) smooth, bay-like disturbances lasting for

approximately 1 hr which occur in both day and night hours;

and (2) abrupt increases, often of large but fluctuating amplitude which occur within a few hours of local midnight.

The smooth enhancements occur almost simultaneously with

the absorption of radiation in a sector of the northern sky.

These effects could be caused by transit of high velocity

streams of charged particles which produce emission from

F region levels and absorption in the E region or below.

The abrupt noise bursts at night are from the northern sky

and seem to be associated with pronounced changes in the

horizontal component of the earth's magnetic field. The

noise may be a form of ""auroral* radiation or may arise from

propagation of solar noise outbursts from the sunlit to the

dark hemisphere. (Met. Abst. 11. 7-164. ) --Authors' abstract.

D-120 Chivers, H. J. A. (Jodrell Bank, Univ. Manchester), Observed variations in the amplitude scintillations of the Cassiopeia (23N5 A) radio source . Journal of Atmospheric and

Terrestrial Physics, London, 19(l):54-64, Sept. 1960. 10

figs. , 2 tables, 6 refs. DLC--

42
Continuous monitoring of the radio source in Cassiopeia

(23N5A) on a frequency of 79 Mc/s has made possible an

analysis of the variations of radio star scintillations observed from Jodrell Bank (latitude 53 N). Monthly average

daily variations are presented as functions of solar time,

and the mean daily variations averaged over a year are evaluated as functions of both solar and sidereal time. An

effect due to the geomagnetic latitude at which the observations were made, is demonstrated. Since records are available for over 4 years, the variations of scintillations with

the sunspot cycle has been studied, and it has been found

that in years of high solar activity scintillations show a strong seasonal dependence with maximum activity at the

equinoxes. When examined over this long period, there is a strong negative correlation between scintillations and

the occurrence of spread F echoes. Evidence has been obtained that the angular size of the Cassiopeia source is

sufficiently large to produce scintillations different from

those expected of a point source. (Met. Abst. 11. 12-33. ) --Author's abstract.

D-121 Chivers, H. J. A. (Univ. of Manchester), The simultaneous

observation of radio star scintillations on different radio

frequencies . Journal of Atmospheric and Terrestrial Physics,

London, 17(3): 181-187, Feb. 1960. fig., 2 tables, 14 refs.

DLC--A comprehensive study of the phenomenon of radio

star scintillation has been made over the range 26 Mc/s to

408 Mc/s, by recording simultaneously on at least two frequencies within this frequency range. With records obtained over a wide range of scintillation conditions, it has

been possible to test the theoretical laws governing the

frequency dependence of scintillation amplitude and rate.

It is established that under extreme conditions these laws

no longer hold. A study of the probability amplitude distribution of scintillations covers a wide range of mean

scintillation amplitudes. The smaller scintillations have

a Gaussian or Rayleigh amplitude distribution, but with

increasing scintillation activity, discontinuities appear in

the distribution obtained. Under the most intense conditions a net attenuation of the source is observed. The

cross correlation coefficient between records has been

determined over a frequency ratio of 3:1 and the results are compatible with those of other workers. (Met. Abst.

11. 12-32. ) --Author's abstract.

D-122 Chivers, H. J. A. (Nuffield Radio Astron. Lab. , Jodrell

Bank, Univ. of Manchester), A statistical study of ionos - pheric drifts measured by the radio star scintillation tech- nique. Journal of Atmospheric and Terrestrial Physics,

21(4):221-224, July 1961. 3 figs. , 8 refs. DLC--

43
Plottings of 627 determinations of drift motions as observed

during the 18 month period of IGY at three Jodrell Bank stations, spaced about 1 km and using 80 Mc/s. Sudden re- versal of direction occurred about 2300 local time and the

complementary reversal at less definite time next day.

--W. N.

D-123 Christiansen, W. N. ; Hindman, J. V.; Little, A. G. et al. , Radio observations of two large solar disturbances. Australian Journal of Scientific Research, Ser. A, Physical

Sciences, 4(l):51-62, March 1951. 6 figs. , 7 tables, 4

refs. DLC--Two exceptionally large radio frequency disturbances of Feb. 17 and 21-22, 1950, were observed in

Australia on seven frequency bands ranging from 62 to

9400 Mc/sec. The time of commencement and the duration of disturbances in the various frequencies are shown

graphically. The relationship to fade-outs, solar and magnetic disturbances is also discussed and illustrated by

records made in Australia. (Met. Abst. 9A-14. )--W. N.

D-124 Christiansen, W. N. and Mathewson, D. S. , Scanning the

sun, with a highly directional array.- Institute of Radio

Engineers, N. Y. , Proceedings, 46(1): 127-131, Jan. 1958.

6 figs. , 12 refs. DLC--A survey is given of the very highly

directive equipment and methods which have been devised

to obtain details of the distribution of radio emission over

the solar disk. A new instrument is described; it operates

on a wave length of 21 cm and gives, for the first time,

radio pictures of the sun. This radio heliograph combines

principles of the multi-element interferometer and the Mills

Cross. It consists of 64 parabolic antennas, 19 ft in diameter, arranged along two lines, each 1240 ft in length, in

form of a cross. Multiple pencil beams about 3 ft wide arc are produced by the system; by means of these the sun is

scanned television wise. The radio heliograph is being

used to produce daily pictures of the sun. (Met. Abst.

unpub. ) --Authors' abstract.

D-125 Chubb, T. A. ; Friedman, H. and Kupperian, J. (U.S. Naval

Res. Lab., Wash., D. C), A Lyman alpha experiment for

the Vanguard satellite. (In: Van Allen, James A. (ed. ),

Scientific uses of earth satellites. Ann Arbor, Univ. of

Michigan Press, 1956. p. 147-151. 2 figs. , 6refs.)DWB,

DLC- -Lyman alpha measurements to determine relation of

sudden ionospheric disturbances to solar flares and radio

fadeouts will be made with equipment developed by N. R. L.

and tested several times in rocket flights. The system

weighs ^600 g and has an operating life of > 500 hours.

It measures a narrow range of spectrum from 1100 to 1340 A,

where 95% of the solar radiation is concentrated in the

44
hydrogen Lyman alpha line. Wiring, storage device for

information, orbital relations, etc. are described and

illustrated. (Met. Abst. 12. 5-62. )--M. R.

D-126 Chubb, T. A. ; Friedman, H. ; Kreplin, R. W. and Kupperian, J. E. , Jr. (all, U. S. Naval Res. Lab., Wash., D.C.),

Lyman alpha and X-ray emissions during a small solar flare.

Journal of Geophysical Research, Wash., D. C. , 62(3):389-

398, Sept. 1957. 4 figs. , 2 tables, 7 refs. DLC -A rocket

instrumented to measure Lyman alpha and X-rays was fired

while a small flare was in progress on June 20, 1956. The

rocket reached peak altitude about 10 min after the flare

was first seen visually. An unusually high X-ray flux was

observed extending to a short wave length limit of 3A. Although the flare was still visible in H C&, Lyman alpha was

not appreciably different from normal. (Met. Abst. 9. 9-118)

--Authors' abstract.

D-127 Chubb, T.A. ; Friedman, H. ; Kreplin, R. W. and Kupperian, J.E. , Jr., Rocket observation of X-ray emission in a

solar flare . Nature, London, 179(4565):861-862, April 27,

1957. 3 refs. DWB--Rocket observations in past 7 years

have shown that quiet sun radiates sufficient X-ray energy

between 10-100 A to account for E region and sufficient UV

(1215 A) for normal D region ionization between 70-90 km.

"Rockoon" ascents are described, fired by radio at 80, 000

ft when a flare occurred; observations were obtained for one

small flare and are discussed. Ionospheric disturbances

aro attributed to X-ray flares. (Met. Abst. 8.7-209.)--

C.E.P.B.

D-128 Chvojkova, Eliska and Link, F. (both, Astron. Inst. , Ondrejov, Czechoslovakia), Echos lunaires sur 20 Mhz et

structure de 1' ionosphere. (Lunar echoes at 20 MHz and

the structure of the ionosphere. ) Bulletin of the Astronomical Institutes of Czechoslovakia, Prague, 5(5):99-104, 1954.

4 figs. , 2 tables, 5 refs. , 16 eqs. Russian summary p. 104.

DLC--A simple theory is proposed for the penetration of

waves coming from outer space. This theory is in better

agreement with measurements made in Australia than BREMMER's theory, as it accounts for attenuation by refraction.

(Met. Abst. 11E-35. )--Transl. of authors' abstract.

D-129 Chvojkova, E. , Propagation of radio waves from cosmical

sources. Nature, London, 181(4602): 105, Jan. 11, 1958.

2 figs. , 3 refs. , 2 eqs. DWB--Examines the propagation of a radio wave from an unionized medium (where its path is

rectilinear) through a spherical ionized shell. The rectilinear part of the ray path is rotated about the center of

45
curvature of the ionized layer by the angle of refraction

t> _ 90° ,ic.2 sin i or

<K *f COS 1,

where i - the angle of incidence of the rectilinear parts of

the ray path; cr - equivalent thickness of the layer; fc - critical frequency of the layer and f - wave frequency.

R depends only on i , fc /f and the content of free electrons present in the layer; it is independent of the electron

distribution within the layer. (Met. Abst. 11E-36. )--N. N.

D-130 Chvojkova, E. (Astronomical Inst. , Czechoslovak Acad,

of Sci. , Prague), Investigation of the ionosphere using

signals from earth satellites. Nature, London, 182(4646):

1362-1363, Nov. 1958. fig. , eq. DWB--Author discusses

some possible effects of the ionosphere on radio signals

from artificial satellites. Various theoretical modes of

long distance propagation around the Earth are considered.

Author believes a satisfactory answer to the question of

what mode of propagation is preferred could probably be

given by a detailed study of the Doppler curves, of direction finding measurements and the variation of band-width

of the received signal when the satellite is deep below the

horizon. (Met. Abst. 12. 7-126. )-M.L. R.

D-131 Chvojkova, E. , The antipodal reception of Sputnik III. Institute of Radio Engineers, N. Y. , Proceedings, 47(6):

1144, June 1959. fig., 4 refs. DWB--Antipodal reception

of Sputnik signals at Stanford, Calif. , on 20 Mc was re- ported by 0„ K. GARRIOTT and O. G. VILLARD between two

afternoon passes, arriving from the SE. Conditions under

which the signal propagates around the world in either of

two ionized layers (a) without reflection or escape, (b)

with escape only, and (c) with return to earth, are discussed and illustrated and an explanation given of why the

antipodal point is the best for return to earth: at this point

transmission can occur with equal probability regardless of

which great circle path is followed. Preferred direction of

arrival depends on ionospheric conditions at points where

ray first touches ionosphere and leaves it, respectively.

Critical frequency of layer must increase from point where

ray first enters ionosphere in order to prevent escape at

next upward penetration of ionosphere. In mid-latitudes

levels containing the same electron density must be more

curved than the earth. No arrival can be expected from

polar directions because of rare polar ionosphere which

would allow escape before mid-latitudes were reached; or from the south, but S"W in forenoon and SE in afternoon

46
would be preferred. SW passage would be less frequent

than SE, since these SW rays would have to pass the re- gion where the critical frequency falls to its morning minimum. In the sunset (P.M.) region turbulence might produce multipath propagation, but this would not destroy

antipodal reception. Therefore, at Stanford frequent antipodal reception in summer afternoons from SE would be ex- pected. (Met. Abst. 11E-37. )--M.R.

D-132 Coates, G.P. (Astronautics Sec. Advanced Projects

Group, Hawker Siddeley Aviation, Ltd. ), Reconnaissance

satellites. Spaceflight, London, 3(3): 100-104, May 1961.

2 figs. DLC --Points out that important value of satellites

in large- scale cloud cover investigations, and military

reconnaissance. Article restricts itself to an investigation of the image forming processes and their possible a- chievements when used in a satellite, and covers the following topics: 1) Orbits of reconnaissance satellites; 2)

Photographic observation; 3) Capability of an existing

camera; 4) Extraction of information from the photographic

satellite; 5) external limitations on photographic system;

and 6) Television and radar system. (Met. Abst. unpub. ) --Author's abstract.

D-133 Goates, Robert J. , Absorption by clouds at 8. 6 mm wavelength. American Physical Society, Bulletin, Ser. 2, 1(2):

98, Feb. 24, 1956. DLC -Clouds produce attenuation of

0-3 db. Simultaneous optical and radio measurements

were taken during a solar eclipse. Abstract of paper from

1956 APS Southwestern meeting, Feb. 24-25, 1956. -- CSIRO abstract. (Unchecked).

D-134 Coates, R.J. , The measurement of atmospheric attenuation at 4. 3 mm. U. S. Naval Research Laboratory, Report

No. 4898, April 2, 1957. DLC--Uses 4.3 mm radio telescope to monitor solar radiation as sun. rose or to measure

thermal radiation from atmosphere. Good agreement between the value obtained for absorption using the two methods. --CSIRO abstract. (Unchecked).

D-135 Coates, R.J. (U. S. Naval Res. Lab., Wash., D.C.),

Measurements of solar radiation and atmospheric attenuation at 4. 3 mm wavelength. Institute of Radio Engineers,

N. Y. , Proceedings, 46(1):122-126, Jan. 1958. 7 figs.

,

table, 10 refs. , 3 eqs. DLC --Solar radiation and atmospheric attenuation were measured at 4. 3 mm wavelength.

The sun was scanned with a radio telescope consisting of a 10 ft precision paraboloid antenna (6. 7 min beamwidth)

and a Dicke type radiometer. Atmospheric attenuations

were determined from the change in received solar radiation

47
with changing elevation of the sun and from direct measurements of the thermal radiation from the atmosphere.

The measured attenuations at the zenith for clear skies

were between 1. 6 and 2. 2 db. At 4, 3 mm wavelength,

the sun (when it is free of sunspots) /appears to be a uniform disk nearly one percent larger than its optical size.

From a large number of measurements over a period of 6

months, the solar brightness temperature was found to be

7000 K with an uncertainty of about 10%. Sunspot regions

are slightly brighter than the quiet areas; the largest observed enhancement is 2%. (Met. Abst. unpub. ) --Author's

abstract.

D-13S Cocconi, Giuseppe and Morrison, Philip (both, Cornell

Univ. , Ithaca, N. Y. ), Searching for interstellar com- munication. Nature, London, 184(4690): 844-846, Sept. 19,

1959. eqs. DLC--The most promising search for radio signals from the possibly existing intelligent beings on other

planets, apparently is the 21 cm\ (1420 Mc/s) of the

neutral hydrogen. It is suggested that preparations be

made to receive radio signals from our fellow space men.

This can be done with our present radic equipment. --W. N.

D-137 Cohen, Marshall H. , Interpretation of radio polarization

data in terms of Faraday rotation. Cornell Univ. School of

Electrical Engineering, Contract AF 19(504) -73, Research

Report EE 295, May 30, 1956. 20 p. 3 figs. , 10 refs. , 27 eqs. --A simple graphical presentation of HATANAKA's

theory of Faraday dispersion due to a finite receiver bandwidth is made. Two-frequency and two-bandwidth experiments to measure dispersion are considered, and the analysis of a two-bandwidth experiment is discussed in detail.

The validity of the high frequency approximation is established for the solar corona, even for the region just above

the plasma level, as long asy ^- 1, and z%0. BUDDEN's

criterion for independence of magneto-ionic modes is applied to two corona models. Using the Allen-Baumbach

formula for electron density and a polar field of one gauss,

the dipole magnetic field model yields uncoupled modes all

the way from the plasma level to the limiting region at the

bottom of the earth's ionosphere. With an irregular dipole

field the modes are uncoupled if the gradient of magnetic

field is very much less than a limit which is proportional

to wavelength, and depends on the height above the photosphere. At {T/r ) = 2 and A. = 1 meter, for example, it is

1 gauss in 25 kilometers. (Met. Abst. 8. 3-344. ) -Author's

abstract.

48
D-138 Cohen, M.H. , Radio astronomy polarization measurements . Institute of Radio Engineers, N. Y. , Proceedings, 46(1):172-

183, Jan. 1958. 8 figs. , 30 refs. , 64 eqs. DLC -This sur- vey includes various polarization measuring schemes discussed in terms of the Stokes parameters. The methods are grouped according to number of component measured. The

Faraday effects discussed include several experiments for

finding the parameters involved. The ionosphere, solar cor- ona, and Crab nebula are discussed in terms of possible

Faraday rotation effects, using Mayer, MacCullough and

Slomaker's 3. 15 cm observations and the optical results to

analyze lower frequency attempts to find polarized radiation. A graphical presentation of Hatanaka's dispersion

theory readily demonstrates that one polarization determination allows limits to be placed on the axial ratio and polarization percentage at the source, and on the ray path integral

of longitudinal magnetic field times electron density. With

suitable assumptions, measurements at two frequencies or with two bandwidths will fix the three quantities. (Met.

Abst. unpub. )- -Author's abstract.

D-139 Cohen, M.H. (Center for Radiophysics and Space Res.,

Cornell Univ. , Ithaca, N. Y. ), High frequency radar echoes

from the Sun. Institute of Radio Engineers, N. Y. , Proceedings, 48(8): 1479, Aug. 1960. 4 refs. DLC --Brief calculation showing how quite small, high limb objects with sufficient field may be seen with a 400 Mc space radar such as

suggested by W. E. Gordon. (Met. Abst. unpub. )--W. N.

D-140 Corcuff, Y. , Choix d'un parametre caracteVisant les sifflements radioelectriques . (Choice of a parameter characterizing radioelectric whistlers.) Annales de Geophysique,

Paris, 15(1): 128-139, Jan. /March 1960. 8 figs. , 6 tables,

6 refs. French and English summaries. DLC--D, the dispersion of the whistlers, which is proportional to the path

length of the energy, has been taken as their character number. The D-dispersion is expressed in the form

*'kVT~fVT~Js

where N - density of ionization along the trajectory, and

H - intensity of the terrestrial magnetic field. The scattering of D depends on the frequency of the waves received.

Consequently, the analysis of the long whistlers leads to

consideration of the dispersion as frequency dependent, and

so to specify the frequency for which it is calculated. 4 kc/s

and zero frequencies seem especially interesting. The methods which may be used to determine the dispersion of any

whistler in both cases are described and discussed. (Met.

Abst. 11. 10-206. )--A.V. and author's abstract.

49
D-141 Cornell University, Ithaca, N. Y. , School of Electrical

Engineering, Statistical analysis of solar noise observational data. Contract W19-122 ac-41, Contract N6onr-26406,

NR 077-321 (Radio astronomy and solar noise). Joint Report

No. 1, May 15, 1950. 26 p. 10 figs. , 5 tables, 7 eqs.

DWB--Solar noise data were obtained almost daily during two

hours local noon time from July to Oct. 1949. Through statistical analysis, some characteristic values were deduced

and are presented in distribution curves featuring the relation between the principal states of the sun (1, very quiet;

2, small activity; 3, medium activity; 4, large activity),

base level, burst power and total power radiated from the

sun at 205 Mc. The curves may be valuable in comparison

with data of the sun's activity to be obtained at other periods of observation. (Met. Abst. 9A-11.)--W. N.

D-142 Cornell University, Ithaca, N. Y. School of Electrical Engineering, Establishment and instrumentation of a Radio Frequency Solar Observatory in the Alamoqordo, New Mexico

area. Contract W19-122 ac-41. Quarterly Reports, No. 6-

12, Sept. 30, 1949-June 30, 1951. Also Final Report, Handbook of Maintenance and Operating Instructions. Dec. 15,

1951. 8 pieces, tables, graphs. DWB--Various phases of

development work in building and equipping this solar observatory are reported in the separate progress reports (1-8).

Report No. 9 gives the results of a conference on solar noise

held at Cornell Univ. , July 12-13, 1950, and some theoretical studies on theory of radio frequency-thermal radiation

from the sun for the case of zero magnetic field, allowing

for variation in index of refraction. Report No. 10 gives

quantitative results of correlation between solar noise and

terrestrial phenomena (magnetic storms, radio fade outs,

etc.). Report No. 11 indicates that continuous daily observations made on 200 and on 50 Mc since Dec. 22, 1950

and coordinated with data obtained at Ithaca, showing identical time and characteristics, indicate solar origins rather

than ionospheric modification as source. Subsequent observations (in Report No. 12) bear out the conclusion that eruptive prominences produce almost simultaneous increase in

radio emissions from the sun at two distant stations. Comparative records are shown. The Final Report comprises a handbook for maintenance, and operating instructions for the

solar radio observatory. Each piece of equipment is described and illustrated, and instructions given for installation, maintenance and operations, including theory. (Met.

Abst. 7. l-44.)-M.R.

50
D-143 Cottony, H. V. and Johler, J. R. , Cosmic radio noise intensities in the VHF band. Institute of Radio Engineers, Proceedings, 40(9): 1053- 1060, Sept. 1952. 8 figs. , 2 tables,

refs. , 7 eqs. DLC --Diurnal, seasonal and frequency characteristics of cosmic radio noise (including both solar and

galactic noise) as affecting the operation of hf and vhf radio

communication systems were investigated in continuous measurements during 1948 and 1949 at the National Bureau of

Standards. Antenna and receiver used in the measurements

and methods of evaluation are described. The apparatus is

shown in diagrams. Sample records and tabulated data of

normal cosmic noise are presented. Normal cosmic noise

intensities were found to be constant. Abnormal high noise

levels were observed in conjunction with unusual solar activity and are shown in transcribed records. (Met. Abst. 9A18.)-G.T.

D-144 Coutrez, Raymond, Radioastronomie. (Radioastronomy.

)

Uccle, Observatoire Royal de Belgique, 1956. 383 p. 170

illus., 18 tables, 451 refs. DLC (QB475.C6). The 10

chapters" of this book were issued successively in Ciel et

Terre, Brussels, 72(1/2), Jan. /Feb. 1956 through 73(5/6),

May/June 1957. --The first chapter of this excellent semitechnical series of articles on radio astronomy takes up the

history of the science, the atmospheric factors affecting the

absorption of the radio waves (excellent schematic diagram

shows factors affecting absorption up to 1000 km in all wave

lengths of the emission spectrum) radio telescopes, places

of origin, and relation to other radiations; II, thermal origin

of waves and, finally, PLANCK 's law. Ch. Ill takes up an- tennas and polarization of waves; Ch. IV circuits wave

guides, interferometers and effect of atmospherics; Ch. V

receivers and amplifiers; Ch. VI, a long review of current

knowledge of all types of radiation from the sun and variations due to sunspote, eruptions, coronal observations, etc.

(95 refs.); Ch. VII concentrates on solar radio radiation in

all its aspects (83 refs.) with many charts and records. Ch.

VIII goes into the physics of galaxies and radio stars (53

refs.) and what we have learned about the differential spiral

motions of nebulas or the Milky Way. The bulk of the literature in this field (up to 1955) is reviewed and ample illustrative material reproduced from these works. Ch. IX takes up

more about galactic and extragalactic radio emissions, and

Ch. X planetary and meteoric radio waves. (Met. Abst.

9A-108.)-M.R.

51
D-145 Covington, Arthur E. , Microwave sky noise. Journal of

Geophysical Research, 55(l):33-37, March 1950. 4 figs.

,

7 refs. MH-BH--Radiation of 2800 mc was received from

empty sky, equivalent to a temperature of ca. 50 K but with

short time bursts from zenith. Examples are described, as- sociated with magnetic disturbances, with aurora overhead

and once with a sudden ionospheric disturbance. (Met.

Abst. 4.9-113.)--C.E.P.B.

D-146 Covington, A.E. (Nat. Res. Council, Ottawa, Canada),

Solar emission at 10 cm wavelength. (In: Paris Symposium

on Radio Astronomy, July-Aug. 1958, (Proceedings), pub.

Stanford Univ. Press, 1959. p. 159-165. 6 figs. , 4 refs.

DLC --Radio emission from the solar disk has been observed

daily at the laboratories of the National Research Council

of Canada in Ottawa, since 1947. The results are interpreted in terms of a daily level of flux and of bursts of noise

that may appear during the day. A plot of the monthly means

for the past 11 yr period, is shown and discussed. Burst

types, simple and complex, as well as impulsive bursts and

long enduring bursts are described. The compound interferometer is described. High resolution drift curves were obtained. The series of drift curves from June 27 to July 1,

1958, show the effect of solar rotation and of the rapidly

changing features upon the solar disk. The drift curves for

the two days after the long enduring burst of June 28 show

several spots placed upon a uniformly raised level. This

has been taken as an indication of the undisturbed solar disk

for the period, and measures 8% wider than the photospheric

disk. (Met. Abst. unpub. )--E.Z.S.

D-147 Covington, A.E. and Harvey, Gladys A. (Radio and Electrical Engineering Div. , National Research Council, Ottawa,

Canada), 10. 7 cm solar noise burst of Nov. 20, 1960. Physical Review Letters, N. Y. , 6(2):51-52, Jan. 15, 1961. fig.,

table, 5 refs. DLC--Two sets of 10.7 cm solar noise observations obtained at the Radio Observatory of the National

Research Council, Ottawa, Canada, are described in this

note. A 13 meter parabolic reflector and a radiometer which

records the solar emission from the whole disk from sunrise

to sunset were used for the first set of observations. The

second set of solar observations was made with a 185 meter

aperture interferometer system with fan shaped beam 1' east

west by 2 north south. Comparison of flare and burst features is presented in tabular form. (Met. Abst. unpub. )--

I.S.

52
D-148 Covington, A.E. and Harvey, G. A. (both, Nat'l. Res.

Council, Ottawa), The visibility of the 10 cm radio emissive region and its application in finding the 10 cm quiet

sun. Astrophysical Journal, Chicago, 132(2) :435-451, Sept.

1960. 10 figs., 3 tables, 13 refs. , 2 eqs. DWB, DLC--

The 10 cm radio emission from 23 individual regions of sunspot activity was measured at the National Research Council,

Ottawa, Canada, with an 8 min of arc fan shaped antenna

beam during a portion of 1952 when relatively few sunspots

were present. On the average, the radio emissive region

appears on the eastern limb from 1 to 2 days before the visible sunspots and remains from 1 to 2 days longer on the

western limb; the radio emission attains its maximum value

2 days before the region reaches the central meridian, and

the sunspot area 4 days before the region reaches the central meridian. For individual regions of radio emission, a scatter diagram of radio flux versus sunspot area shows that

there is a component of emission which is independent of area. This has led to a new expression in which the total

daily flux from the solar disk is expressed empirically as

the sun of three components: the first is the solar background; the second is related to the number of sunspot groups

upon the disk; and the third is related to the area of the sunspots present. Values for the quiet sun for the years 1948-

1956 have been derived. (Met. Abst. 1 1L -87. )- -Authors'

abstract.

D-149 Covington, A.E. ; Harvey, G. A. and McNarry, L. R. , The

solar noise burst of Nov. 12, 1960. Canadian Journal of

Physics, Ottawa, 39(4): 635-636, April 1961. 2 figs. DWB,

DLC--This is a note on the intense burst of solar radio noise

which accompanied the flare of Nov. 12, 1960. The observations made at the discrete frequencies of 2800 Mc/s and 48

Mc/s at the Radio Observatory of the Radio and Electrical

Engineering Div. of the National Research Council are presented, and the related data described. A reconstruction of

the high frequency burst is shown in graphic form and a photo

plate shows a portion of the low frequency record. (Met.

Abst. unpub. )--I. S.

D-150 Cox, H. W. , Radio propagation and the Sun. British Astronomical Association, Journal, 55(5):92-93, May 1946. DLC--

Interference in the 4-6 m \ band in Great Britain and elsewhere was caused by solar flares during the latter part of

Feb. and the beginning of March 1942. The brief review also

includes effects on radio wave reflection from various ionospheric layers as observed in many parts of the world during

the solar eclipse July 9, 1945. --W. N.

53
D-151 Cranshaw, T.E. ; Galbraith, W. and Porter, N. A. , Cosmic

ray observations during the flare of Feb. 23, 1956. Journal

of Atmospheric and Terrestrial Physics, London, 8(4/5):274-

276, May 1956. 3 figs. Also: Lambie, M. and Elliot, H.

,

Cosmic rays and the solar flare of Feb. 23, 1956. p. 277-

278. table, ref. Also: Marsden, P.L. ; Berry, J. W. ; Fieldhouse, P. and Wilson, J. G. , Variation of cosmic ray

nucleon intensity during the disturbance of Feb. 23, 1956.

p. 278-281. fig., 2 tables, 3 refs. Also: Belrose, J. S. ; Devenport, M.H. and Weekes, K. , Some unusual radio observations made on Feb. 23, 1956. p. 281-286. 5 figs. , 4

refs. Also: Gold, T. and Palmer, D. R. , The solar outburst Feb. 23, 1956: observations by the Royal Greenwich

Observatory, p. 287-291. 4 figs. , table, 2 refs. Also:

Ellison, M.A. and Reid, J. H. , A long wave anomaly as- sociated with the arrival of cosmic ray particles of solar origin on Feb. 23, 1956. p. 291-293. 2 figs. DWB-Records

at Harwell showed a sudden rise of coincidence rate to three

times normal at 0345 + 2 min on Feb. 23. In London the increase was 120% at 0345 - 0400, and at Leeds the nucleon

intensity rose to 47 times normal in the same period. At

Cambridge the sky wave on 16 and 71 Kc/s behaved abnormally and there was a sudden drop in average intensity of atmospherics at 0345; these are attributed to a sudden change

in the height of reflection and amplitude. Conditions were

still markedly abnormal at sunrise but recovered during the

night. Cosmic ray counts and atmospherics at Hurstmonceux showed similar fluctuations. At Abinger a magnetic

storm began suddenly on Feb. 25. A photograph of the flare

at Kodaikanal is included. At Edinburgh long wave atmospherics decreased suddenly but galactic noise was steady.

(Met. Abst. 7. 10-1.)-C.E.P.B.

D-152 Crary, J. H. ; Helliwell, R.A. (both, Stanford Univ. ) and

Chase, R.F. (Boeing Airplane Co. , Seattle Wash. ),

Stanford-Seattle whistler observations. Journal of Geophysical Research, Wash., D.C., 61(l):35-44, March 1956. 6

figs., 4 refs., 4 eqs. DLC --Simultaneous observations of

times of occurrence of whistlers were made at Seattle, Wash,

and Stanford, Calif. , two hours every week from Oct. 1951

to Oct. 1952. Times were measured to an accuracy of about

+ 1 sec. The objective was to determine the percentage of

whistlers received at either station which were coincident at

both. A total of 318 whistlers was received at Stanford and

283 at Seattle during simultaneous observations. The occur- rence rate of whistlers (during a two hour period) varied from

to roughly 55 per hour at Stanford and from to 70 per hour

at Seattle. The correlation between the occurrence rates was

poor. The number of true coincidences was found by subtracting the number of chance coincidences from the number

54
of total coincidences. A method for computing the number

of chance coincidences from a knowledge of the time intervals between whistlers at the one station was derived. The

analysis showed that approximately 22% were observed simultaneously at both stations. This result is examined in re- lation to possible theories of whistler origin and propagation,

and is shown to support the Storey-Eckersley theory. (Met.

Abst. 8.3-95.) --Authors' abstract.

D-153 Croft, T. A. and Villard, O. G. , Jr. (Stanford Univ. , Radio

Sci. Lab., Calif.), An HF radar search for possible effects

of earth satellites upon the upper atmosphere. Journal of

Geophysical Research, 66(10):3109-3118, Oct. 1961. 8

figs. , 6 refs. DLC--Describes control experiments to check

ionospheric disturbances assumed to be caused by the passage of artificial satellites. Equipment and method used to

record 133 passages of Sputnik III and 6 of Echo I are described. The disturbances observed, without exception, were

of natural origin. --W. N.

D-154 Dagg, M. , The correlation of radio star scintillation phenomena with geomagnetic disturbances and the mechanism of

motion of the ionospheric irregularities in the F region.

Journal of Atmospheric and Terrestrial Physics, 10(4):194-

203, 1957. 9 figs. , 13 refs. DWB--F-region drift velocities

measured by scintillations of radio source in Cassiopeia at

Jodrell Bank showed marked correlation with K- indices (mean

of Eskdalemuir and Lerwick). Rapid changes of fluctuation,

compared with magnetograms, showed close correlation of

rate with V, and on some occasions of amplitude with H.

Results support MARTYN's theory that observed drifts in F

region are not air motions but are due to interaction of earth's

magnetic field with an electric field from lower levels. (Met.

Abst. 8.8-189.)-C.E.P.B.

D-155 Dagg, M. , Diurnal variations of radio star scintillations , spread F, and geomagnetic activity. Journal of Atmospheric

and Terrestrial Physics, 10(4): 204-214, 1957. 7 figs. , 11

refs. DWB--Aerial at Jodrell Bank directed at Cassiopeia,

and receiver, are described and scintillation records shown.

Monthly and average diurnal variations of scintillation oc- currence and amplitude, occurrence of spread F at Inverness,

and summation of magnetic K indices, are shown for Aug.

1954-July 1955. Maximum scintillation occurs about 2130,

several hours earlier than spread F maximum. A marked cor- relation is found between scintillation rate amplitude and

geomagnetic activity. (Met. Abst. 8. 8-190. )--C.E. P.B.

55
D-156 Dagg, M. (East African Agri. and For. Res. Org., Kenya),

The origin of the ionospheric irregularities responsible for

radio star scintillations and spread F, Pt. 1, Review of existing theories. Journal of Atmospheric and Terrestrial Physics, London, 11(3/4): 133-138, 1957. 24 refs. DLC--The

present state of knowledge about the irregularities responsible for radio star scintillations is summarized, and the existing theories of the origin of these irregularities are discussed. All of the suggestions are shown to be inadequate

to explain the observed features of scintillations and spread

F. It is shown that any ionizing agent from outside the

earth's atmosphere is unlikely to be responsible for the ionospheric irregularities that cause radio star scintillations, and

that the mechanism for their production must be sought in the

terrestrial atmosphere. (Met. Abst. 9. 10-167. )--Author's

abstract.

D-157 Dagg, M. (East African Agri. and For. Res. Org. , Kenya),

The origin of the ionospheric irregularities responsible for

radio star scintillations and spread F, Pt. 2, Turbulent mo- tion in the dynamo region. Journal of Atmospheric and Terrestrial Physics, London, li(3/4): 139-150, 1957. 5 figs.

,

22 refs. , eqs. DLC--A theory is presented which attributes

the occurrence of ionospheric irregularities in the F region

to turbulent wind motion in the dynamo region at a height of

110-150 km. The resulting turbulent component of the electric potential field produced is communicated to the F region,

as suggested by MARTYN (1955), where magneto-electric

forces then cause the ionization to form eddies. It is suggested that the absence of daytime scintillations is due to

the inhibition of turbulent flow by large temperature gradients

during the day. The theory is then compared in detail with

observations and shown to be capable of explaining all the

major features of radio star scintillations, together with such

diverse results as. the long term' correlation of scintillation

amplitude with magnetic activity and the variation in the oc- currence of spread F and scintillations at different parts of

the earth over the sunspot cycle. (Met. Abst. 9. 10-168.)--

Author's abstract.

D-158 Daniels, Fred B. and Bauer, Siegfried J. (both, U.S. Army

Signal Engineering Labs. , Fort Monmouth, N. J. ), Measurement of the ionospheric Faraday effect by radio waves re- flected from the moon. Nature, London, 181(4620): 1392-1393,

May 17, 1958. 2 figs. , 2 eqs. DWB-Using the rotation of

the plane of polarization of radio echoes from the moon, it is

possible to determine the change in total electron content of

the ionosphere. This is a report on such an experiment made

the night of Jan. 8-9, 1958. Results indicated a change about

56
2. 2 times that computed for a parabolic layer using vertical

sounding data recorded at the transmitting site. (Met. Abst.

11F-25. ) -Based on Physics Abstracts No. 5543, 1958.

D-159 Daniels, F.B. and Bauer, S.J. , Faraday fading of earth

satellite signals. Nature, London, 182(4635): 599, Aug. 30,

1958. 2 refs. , eq. DWB--Note on British attempts to estimate ionospheric integral electron content up to the satellite's height by means of rate of fading due to the Faraday

effect. Too high values were obtained which may be ex- plained by the omission of the satellite's radial velocity

component in the theoretical expressions. (Met. Abst.

llE-40.)--W. N.

D-160 Daniels, F.B. and Bauer, S.J. , The ionospheric Faraday

effect and its applications . Franklin Institute, Journal,

267(3): 187-200, March 1959. 7 figs. , 8 refs. , 7 eqs. DLC--

The theory and Faraday effects are outlined and analyzed.

Since the rate of fading of satellite signals depend on both

integrated and local electron density at the height of the

satellite, these quantities are determinable if satellite transmission is simultaneously received at two or more stations.

The discussion includes expressions for the fading rate and

effects of orbital parameters. --W. N.

D-161 Daniels, F. B. , Radar determination of the scattering properties of the moon. Nature, London, 187(4735) :399, July

30, 1960. 2 refs. , 4 eqs. DLC--J. Feinstein's equations,

in which he used Huygen's principle to study the general

problem of reflection from a plane surface having random ir- regularities that are functions, both of space coordinates

and of time, were applied with minor modifications to lunar

radio echoes. (Met. Abst. 8J-49. )--S. N.

D-162 Das, A. K. and Sethumadhavan, K. , Eruptive prominence

of Feb. 26, 1953, and associated radio noise burst. Nature,

London, 172(4375) :446-447, Sept. 5, 1953. 4 figs. , 3 refs.

Also: Davies, R.D. , Radio observations at the time of an

ascending solar prominence . Ibid. , p. 447-448. DWB--Both

notes refer to a prominence which broke off from sun's sur- face about 0510 hr. Spectrograms at Kodaikanal, India, show

details of spiral motion and structure. Three solar noise

bursts were recorded on 100 Mc/s at Kodaikanal and on several wave lengths at Sydney, Australia. (Met. Abst. 9A-28)

-C.E.P.B.

57
D-163 Das, A. K. and Narayana, J. V. (both, Kodaikanal Obs. , Kodaikanal), Momentary bursts of cosmic radiation. Indian

Journal of Meteorology and Geophysics, New Delhi, 11(1):

50-56, Jan. 1960. table, 6 refs. DWB, DLC--A standard

Kolhorster cosmic ray apparatus with photographic recorder

has been in continuous operation since March 1956. A table

gives the dates of momentary bursts of cosmic radiation,

the time, voltage drop during burst, solar flares, solar radio

emissions and radio fadeouts which occurred simultaneously

or within reasonable time to be thought to be associated. It seems probable that every solar flare is accompanied by

emission of cosmic rays and these are greatly dispersed by

the local magnetic field of the spots and are further deviated

by the magnetic field of the earth. (Met. Abst. 11. 11-41. ) --£. Lkm S.

D-164 Dauvillier, Alexandre, Puissant flux solaire nocturne de

rayons cosmigues penetrants . (Powerful flux of penetrating

cosmic rays from the sun at night. ) Academie des Sciences,

Paris, Comptes Rendus, 242(11): 1399-1401, March 12, 1956.

2 refs. Also: Bureau, Robert and Bertrand, Maurice, Perturbation exceptionnelle du rayonnement solaire le 23 fevrier

1956 vers 0345 T. U. (Unusual disturbance of solar radiation

on Feb. 23, 1956 around 0345 G. m. t. ) Ibid, 242(16):2025-

2027, April 16, 1956. fig. DLC--A solar cosmic ray flux

of unusual intensity was measured by DAUVILLIER at Bagneres on Feb. 23, 1956, starting at 03 h 43 min. The phenomenon was observed on three instruments (including a radio

telescope) sensible to various cosmic ray components. This

recording of high energy positive nuclei in the dark hemisphere is offered as definite proof of a geomagnetic effect.

It also appears that a midget star like the sun is capable of

emitting particles having far higher energy than assumed

previously. BUREAU and BERTRAND report decreases in

radio propagation at various locations in France (especially

on 11, 000 m wave length) which coincided almost perfectly

with the cosmic ray flux observed by DAUVILLIER. He also

mentions ionospheric and radio propagation anomalies observed at various stations throughout the world. (Met. Abst.

91-18. )-G.T.

D-165 Davies, J. G. ; Evans, J. V. ; Evans, S. et al. (all, Jodrell

Exp. Station, Manchester Univ. ), Radar observations of the

second Russian earth satellite (Sputnik II 1957/ff ). Royal

Society of London, Proceedings, Ser. A, 250( 1262) :367-376,

March 24, 1959. 3 figs. , 2 tables, 7 refs. DWB, DLC--

A description is given of the radar observations of the second Russian earth satellite (Sputnik II, 1957/? ) using the

80 m steerable radio telescope at Jodrell Bank on frequencies

58
of 36 and 100 Mc/s. An investigation of the fading characteristics of the echoes suggests that the observed fading

arises from (i) Faraday rotation, (ii) ionospheric scintillation, (iii) rotation of the satellite. Evidence is produced

which suggests that (i) was not the principal cause of the

fading under the conditions of these experiments, and that

(ii) the scintillation effects arise in a diffracting region at a height not greater than 220 km, which is contrary to the

results obtained in the study of the scintillation of radio

stars. The effect (iii) seems to have been responsible for

most of the observed fading and it would appear that the

satellite was rotating about an axis which was nearly perpendicular to its major axis. The effective scattering area

of the satellite at 100 Mc/s was of the order of 15 m^ but

at 36 Mc/s it varied between 10 and 500 m^. From this it is concluded that the satellite was a long object having a

reradiation polar diagram with one major and many minor

lobes. No evidence was obtained to indicate that the satellite produced any ionization detectable at these frequencies, although it was observed as late as the third orbit before final burn up. Successful contacts were made on only

about one-quarter of the transits observed. It has been possible to establish in retrospect whether the satellite passed

through the main beam of the aerial. Such an analysis shows

that on many occasions where no echoes were obtained the

telescope was correctly positioned, and the failure to obtain

echoes on these occasions is attributed to deep fading introduced by the rotation of the satellite and by Faraday rotation

of the plane of the radio waves. (Met. Abst. 11. 2-76.)--

Authors' abstract.

D-166 Davies, Kenneth (Nat'l. Bur. of Stands. , Boulder, Colo.),

A study of 2 Mc/s ionospheric absorption measurements at

high latitudes . Journal of Geophysical Research, Wash.

,

D.C., 65(8):2285-2294, Aug. 1960. 7 figs., 3 tables, 20

refs. , 7 eqs. DLC --Ionospheric absorption (L) at high latitudes is studied using the published data on 2. Mc/s at

five Canadian stations during 1957 and 1958. The seasonal

and diurnal variations are considered, and it is found that a

pronounced winter anomaly in noon absorption occurs at

Churchill but not at Resolute Bay. The diurnal variations

indicate that the dependence of absorption on solar zenith

angle decreases with increase of latitude. The distribution

of midnight absorption with latitude shows that, although

the maximum occurs in the auroral zone, high absorption is

also encountered over the polar cap. A study of the duration of long lasting blackouts shows that in summer the duration is longer as the latitude increases. (Met. Abst. 11. 11-

50. )- -Author's abstract.

59
D-167 Davies, Rodney Deane, An analysis of bursts of solar

radio emission and their association with solar and terrestrial phenomena. Royal Astronomical Society, Monthly

Notices, 114(1) :74-92, 1954. 14 figs. , 7 tables, 20 refs.

DWB--Solar radio emission records on seven frequencies in

the range SO to 10, 000 Mc/s were studied over a period of

18 months. The analysis, which includes a number of histograms, shows that many of the properties of bursts change

with frequency. A study of the time delay between bursts

on different frequencies revealed that 3000 Mc/s bursts

often occur first; a simultaneous up and down movement of

ionized material from the level of zero refractive index at

that frequency is postulated. It is found that bursts were

more frequent than flares, fadeouts and crotchets and that

they almost always accompanied these effects. The commencement of bursts appears to be simultaneous with that

of flares and crotchets but precedes that of fadeouts by

about two minutes. In addition, there is a rough correlation between the intensity of bursts, flares, fadeouts and

crotchets. (Met. Abst. 6. 9-182. ) -Author's abstract.

D-168 Davies, R.D. and Palmer, H.P. , Radio studies of the

universe. Foreword by A. C. B.Lovell. Princeton, N. J.

,

Van Nostrand, 1959. 200 p. figs. , photos, bibliog. p. 189-

192. DLC (QB475. D3). Review in Weather, London, 14(11):

370, Nov. 1959. --This book, written for the "intelligent nonscientist, » contains a discussion of astronomy and an outline of optical astronomy. In addition to the chapters on

radio methods of observation, studies of radio sources, the

radio universe, radio waves from the milky way and the sun,

it contains explanations on exploring the planetary system

with radar and probing the Earth's high atmosphere. An appendix provides the reader with a brief explanation of basic

concepts such as the Doppler shift, blackbody radiation,

and the Faraday effect. Finally, a glossary of terms used

in context is included. Separate bibliography for each

chapter. (Met. Abst. 11. 12-36. )--E.Z. S.

D-169 De Feiter, L. D. , De exosfeer: atmosferische fluittoonties

en radiostraling uit de aardse korona . (The exosphere: atmospheric whistlers and radio radiation from earth's corona. ) Hemel en Dampkring, The Hague, 58(7/8): 161-181, July/Aug.

1960. 10 figs. DWB, DLC--Radio waves follow remarkable

paths when they cross the earth's atmosphere; they move from

one hemisphere to the other. Related to atmospheric whistlers are the very low frequency emissions in the earth's atmos

phere caused by magnetic storms and polar light. The study

of the two phenomena has been of great interest in the re- search on the exosphere. The author gives an historical ac- count of whistlers, observed for the first time in 1888 in

60
D-170

D-171

Austria, and also describes the instrumentation, especially

the antenna. STOREY differentiated between short and long

whistlers and the article explains this difference. Whistler

phenomenon and nose whistlers are explained theoretically;

the relation between whistlers and the outer parts of the atmosphere is shown. One chapter gives a very good description of the exosphere and of rising whistlers, odd shaped

whistlers, hooks, etc. The article ends by giving some con- sideration to the observations made in this field. (Met.

Abst. 12. 5-116. )--A.V.

de Groot, T. (Sonnenborgh Obs. , Utrecht, Netherlands),

Spectra of short lived transients in solar noise at 400 Mc/s. (In: Paris Symposium on Radio Astronomy, July-Aug. 1958,

(Proceedings), pub. Stanford Univ. Press, 1959. p. 245-

247. 2 figs. DLC--The solar work at the radio observatory

near Dwingeloo is concentrated on the investigation of re- latively small bursts which, having the aspect of elementary phenomena, could give some insight into the way in

which they are related to their immediate cause. The duration of single bursts and their spectral profiles were investigated. The spectral profiles obtained thus far have

half-power bandwidths ranging from 4 to more than 14 Mc/s,

about half of them have a Gaussian shape and an average

bandwidth of + 2. 5 Mc/s, the remainder consist.of various

irregular forms with bandwidths of the order of 12 Mc/s.

The spectral work illustrates the use of narrow band spectrometry with a low time constant as a means of getting a

detailed knowledge of the microbursts. Comparison with

simultaneously obtained broad-band spectra will be necessary to complete the picture. (Met. Abst. unpub. )--£. Z. S.

de Groot, T., Dynamic spectra and polarization of small

bursts in solar radio emission. Bulletin of the Astronomical

Institutes of the Netherlands, 15(502): 229-236, Dec. 30,

1960. 12 figs. , 4 refs. DLC--High speed recordings of

noise storms and storm bursts were taken with an 8 channel

radio polarimeter with a total band width of 15 Mc/s at 390,

330, and 274 Mc/s, respectively. It appears that the intensity of single storm bursts can be written as I (f, t) =

I, (f). I«(t), where I, and I« are symmetric profiles with

average half power widths of 6 Mc/s and . 18, respectively. These values are independent of the frequency in this

region. Noise storms may be regarded as a superposition of

these single bursts in the f, t-plane with a high density.

Lesser burst activity, prevalent at the higher frequencies,

suggests a clustering tendency of storm bursts, which may

be due to less favorable transmission conditions in the

solar corona, allowing only glimpses of noise storms to be

61
observed. An individual noise storm is, among other things,

characterized by peculiarities in the shape of its complex

bursts, according to the way in which single storm bursts

are superposed. Polarization does not seem to be an inherent property of noise storms. Sometimes they are accompanied by incidentally occurring unpolarized broad banded

bursts with durations of the order of a second and time

shifts from - 0. 02 Mc/s, which may be weak type Ill's.

(Met. Abst. unpub. )- -Author's abstract.

D-172 Dellinger, John Howard (U.S.Nat'l. Bur. of Standards,

Radio Section), A new cosmic phenomenon. Science,

82(2128):351, Oct. 11, 1935. DLC--Brief note on the phenomenon involving all HF radio transmissions over the illuminated half of the globe. Sudden disappearance and reappearance of radio communication at 54 day intervals permits

forecasting of the phenomenon, apparently caused by some

solar emanation lasting only a few minutes. Regular observations and reports on this phenomenon are suggested.

' --W. N.

D-173 Dellinger, J. H. , Sudden disturbances of the ionosphere.

National Bureau of Standards, Journal of Research, 19(2):

111-114, Aug. 1937. 10 figs. , table, 30 refs. DLC«This

is the first detailed report on the solar effect, discovered

by the author in 1935, manifesting itself as a complete fading of HF radio communication for a period of minutes up to

hours, and by perturbations of terrestrial magnetism and

earth currents. The report is based on world wide cooperation, by analyzing the records of the several contributing

stations. --W. N.

D-174 Dellinger, J. H. , International cooperation in radio re- search - - URSI and IRE. Institute of Radio Research, N. Y.

,

Proceedings, 44(7):866-872, July 1956. DLC--URSI (Int.Sci.

Radio Union) deals with scientific and IRE with engineering

and development aspects of radio science. IRE was established in 1912 in the U.S. , whereas URSI was established

in 1919 at the same time as IUGG under the Int. Research

Council (later ICSU). Five presidents include A. E. KENNELLY (1932-4) and E. V. APPLETON (1934-52). Places and

dates of 11 General Assemblies 1922-1954, and the 7 Commissions are listed (Sec. II. is Tropospheric Propagation;

III. Ionospheric Propagation; IV. Terrestrial Noise; V. Radio Astronomy). National Committees, the work and structure of the U.S. National Committee and some of the accomplishments of URSI, including the idea for IGY in 1957/8,

are described. Joint committees with IUGG, etc. , accomplish much in ionospheric and related research. (Met. Abst.

9A-109.)--M.R.

62
D-175 De Mastus, Howard and Wood, Marion (Sacramento Peak

Obs. f Nat'l. Bur. of Standards, Boulder, Colo.), Short

wave fadeouts without reported flares. Journal of Geophysical Research, 65(2):609-611, Feb. 1960. fig. , 2 tables,

2 refs. DLC--A reexamination of Sacramento Peak flare

patrol films obtained on days when SWF occurred without

flares reported. Of the 15 cases examined, 12 were closely

time associated with outstanding H CO events; 2 so poor as

to render statement useless and one without association.

--W. N.

D-176 de Mendonca, F. ; Villard, O. G. , Jr. and Garriot, O. K.

(all, Radioscience Lab. , Stanford Univ. , Stanford, Calif. ),

Some characteristics of the signal received from 1958 $ Z . Institute of Radio Engineers, N. Y. , Proceedings, 48(12):

2028-2030, Dec. 1960. 4 figs. , table, 7 refs. DLC--The

existence of specific irregularities such as in the scintillation, field alignment and skip distance in the electron

density of the ionosphere is discussed as a result of the

spectrum analysis of the signals received from 1958 5 2.

During June 1958 through April 1959 over 200 passages of

the satellite and its vertical incidence ionograms were re- corded at Stanford University. Various combinations of

scintillation were made and are tabulated. They show that

scintillation always accompanied spread F. Some backscatter records obtained also show echoes from field aligned

ionization at a range of about 1000 km to the north. The re- port illustrates the build-ups, in pairs, of complex signal

strength variations as the satellite passed into the "skip*

region at a height below the F region maximum density.

Such a paired formation is explained on the basis of magneto-ionic theory and depends upon the magnitude of the

component of the earth's magnetic field resolved along the

direction of the ray at the reflection height in the ionosphere. —N. N.

D-177 Denisse, Jean-Francois, Relation entre l'activite geomagnetique et ractivite^radioelectrigue solaire. (Relation between geomagnetic activity and radioelectric activity.

)

Annales de Geophysique, Paris, 8(l):55-64, Jan. /March

1952. 3 figs. , 13 refs. English summary p. 55. DWB--

Following daily measurements of solar radiation on 158

Mc/s, made at Marcoussis from 1948 to 1950, the effect

of solar active centers on radioelectric and geomagnetic

intensity is analyzed. Among solar energy centers,discrimination is made between radioelectrically active and inactive centers. The former are found to be followed 2-3 days

after their passage through the central solar meridian by increased geomagnetic activity, while the latter have no geomagnetic effect. (Met. Abst. 6. 6-214. )--G. T.

63
D-178 Denisse, J. F. , Les centres solaires d'activite' radical ec- trigue et leur influence sur 1 ' activity geomagnetique. (Solar

centers of radioelectric activity and their influence on geomagnetic activity. ) Ciel et Terre, 69(3/4): 53-67, March/

April 1953. 6 figs. , table, 15 refs. DWB, DLC-Major

centers of solar activity are classified into groups A (radio

emissive centers) and B (non-emissive). From data obtained

in continuous measurements of so^ar radioelectric activity

on 158 Mc at the Laboratoire des Etudes de la Marine &

Marcoussis (Paris) since 1948, centers of group A are se- lected on the basis of an index accounting for intensity and

variability. A correlation is established between solar ra- dioelectric emission and subsequent intensification of geomagnetic disturbances. It is also shown that solar centers

of group B have an attenuating effect on geomagnetic activity. The applicability of these results to the prediction of

geomagnetic and ionospheric disturbances is suggested.

Correlations between magnetic and solar activity analyzed

by other authors are discussed. (Met. Abst. 9K-23. )--

G.T.

D-179 Denisse, J. F. , Relations entre les phenomenes solaires et

terrestres. (Relations between solar and terrestrial phenomena. ) Academie des Sciences, Paris, Comptes Rendus,

236(19): 1856-1858, May 11, 1953. 2 figs. DWB--In an

earlier paper (see ref. D-177) the author and his collaborators produced evidence to the effect that sunspots involving

strong radioelectricity are accompanied by an increase of

geomagnetic activity, while a decrease of geomagnetic activity takes place when sunspots (even if they are large) are

electrically inactive. In support of this theory, the author

now presents two curves based on a more extensive statistical material (1948-1950) than those presented in the previous papers. Details regarding the relative time of increasing and decreasing magnetic and electric activity are discussed. (Met. Abst. 9K-24. )--G.T.

D-180 de Witt, J. H. and Stodola, E. K. , Detection of radio signals reflected from the moon. Institute of Radio Engineers,

Proceedings, 37(3): 229-242, March 1949. 18 figs. , 4 refs.

,

36 eqs. DLC- -Describes research work at U.S. Army Signal

Corps at Evans Signal Laboratory, Belmar, N. J. , since 1945

and up to date. Moon reflections were obtained with equipment for which formulas and curves, showing the attenuation

between transmitting and receiving antennas, are presented

and discussed. Quantitative treatment is given of the moon

reflected pulse shape and intensity. --W. N.

64
D-181 Dicke, Robert H. and Beringer, Robert, Microwave radiation from the sun and moon. Astrophysics Journal, Astrophysics Journal, 103(3): 375-376, May 1946. fig. DLC--

A radiometer provided with an 18 in. parabolic reflector

aerial of gain 6000 was used to measure the sun's electromagnetic radiation at a wavelength of 1. 25 cm during the

partial eclipse of July 9, 1945. The observed intensities

fit well with those obtained by assuming the sun in this

radio region to a uniform disc of optical size at 10, 000 K.

Similar measurements on the nearly full moon give an effective temperature of 292 K.

D-182 Dieminger, Walter (Univ. of Gettingen), The electromag- netic environment of the atmosphere and nearer space.

International Symposium on the physics and Medicine of the

Atmosphere and Space, San Antonio, Texas, Nov. 1958,

Proceedings of the 2nd Symposium, pub. N. Y. , John Wiley,

1960. p. 91-99. 5 figs. , 19 refs. DLC, DWB--A discussion of the electromagnetic environment of the atmosphere

and nearer space. The first part of the chapter is confined

to a discussion of the facts brought to light by the investigation of the phenomena on the ground and in the upper atmosphere. In the second part some of the guesses about

conditions in interplanetary space are mentioned. From the

point of view of space travel it may be concluded that the

electromagnetic environment is not a serious obstacle to

interplanetary travel. The magnetic fields and the electric

currents involved are efficient on an interplanetary scale

only. Measured in earthly dimensions, they are far too

weak. Also, the densities of slow corpuscular streams

from the sun and of the ring current are far too small to affect a space vehicle in a catastrophic manner. However,

there might be a noticeable influence on the drag in regions

of very low density. The screening effect of the ionosphere

for wavelengths above a certain limit would make it necessary for communication systems to be based on very high

frequency in space travel, and the space traveller will have

to renounce the reception of most broadcasting stations as

soon as he passes the ionosphere. On the other hand, the

sky will be open for all radio frequency emissions originating from stars and galaxies. (Met. Abst. unpub. )--E. Z. S.

D-183 Dinger, Harold E. (Naval Research Lab. , Communication

Branch, Radio Div. ), Whistling atmospherics . U.S. Naval

Research Laboratory NRL Report 4825, Sept. 14, 1956. 37 p.

numerous figs. , 20 refs. , 2 eqs. Price: $1. 25. DWB--Since

1953 NRL has been observing and recording audio frequency

atmospherics and their correlation with other geophysical

phenomena. Beginning in April 1955, the diurnal variation

in both whistler activity and the occurrence of "dawn chorus*

65
has been determined. Whistler coincidence at several

locations has been recorded in an attempt to prove

L. R.O. STOREY's theory on the mode of propagation of

these atmospherics. Many whistlers of unusual character

have been spectro-analyzed for the purpose of extending

present theory io cover the general case. Plans have been

formulated for synoptic observations at a number of selected

locations during the International Geophysical Year. (Met.

Abst. 9.4-281.) --Author's abstract.

D-184 Dodson, Helen W. (McMath-Hulbert Obs. Univ. of Mich.),

Relations between flares and 1. 5 meter solar radiation. International Council of Scientific Unions, Brussels, Commission for the Study of Solar and Terrestrial Relationships,

Rome, Sept. 1952, Proces -Verbal et Communications, pub.

1953. p. 12. DWB--A brief note that disturbances on 1. 5

m are associated with H CO flares. The typical form is a distinct "early* burst at the commencement of the flare and a "late* disturbance at or after maximum HOC radiation. The

early burst coincides with high velocity ejection of hydrogen

and ionized calcium. (Met. Abst. 9A-30. )--C.E. P. B.

D-185 Dodson, H. W. ; Hedeman, E. Ruth and Owren, Leif (McMath

Hulbert Obs. , Michigan Univ. and School of Elec. Eng.

,

Cornell Univ. ), Solar flares and associated 200 Mc/s radiation. Astrophysical Journal, 118(2): 169-196, Sept. 1953.

10 figs. , 12 tables, foot-refs. DWB-Study of 200 Mc/s

solar radiation for the times of 194 flares indicates distinctive radio events associated with 78% of the flares. The

flare associated distinctive events can be divided into ten

descriptive types or categories: major burst, major burst

with second part, minor burst, minor burst with second part,

micro burst, group of bursts, series of bursts, noise storm

in progress, onset of noise storm, and rise in base level.

In addition, there is the designation "null, " or no distinctive event. Consideration of the time relationships between

flares and 200 Mc/sec events suggests that two quite different types of phenomena may be represented in the flare

associated 200 Mc/sec radiation. The first or "early" phenomena includes very sudden, relatively isolated, burstlike

features which occur close to the time of start of the flare.

The second or "late" phenomenon includes the more gradual

rises in base level and onsets of noise storms. These

usually start at or after the time of flare maximum. The

"early" and "late" phenomena can occur in conjunction with

each other, or either of the two can occur separately. The

importance of the flare, position on the solar disk, and ac- companying ionospheric disturbances are considered with

respect to the form and energy excess of the flare associated

200 Mc/sec events. The various aspects of the complex

66
flare phenomenon, as observed photographically and visually, are discussed. An association is suggested between the

high-velocity ejections observed at the onset of certain

flares and the occurrence of a major burst at 200 Mc/sec.

From the point of view of the parameters considered in this

paper, the flares for which there were no distinctive events

on the 200 Mc/sec records constitute a random sample from

the entire set of 194 flares. (Met. Abst. 9A-31. )--Authors'

abstract.

D-186 Dodson, H. W. ; Hederman, E. R. (McMath-Hulbert Obs.

,

Michigan Univ. ) and Covington, A.E. (Nat'l. Res. Council, Canada), Solar flares and associated 2800 Mc/sec

(10. 7 cm) radiation. Astrophysical Journal, 119(3): 541 -563,

May 1954. 13 figs. , 5 tables. DWB-Study of 2800 Mc/sec

solar radiation at the time of 213 flares and 173 subflares

has shown distinctive radio events associated with 57% of

the flares and 19% of the subflares. The flare-associated

distinctive events at 2800 Mc/sec can be described by es- sentially the same types and categories already used to re- port outstanding disturbances at this radio frequency: single

bursts; single-simple bursts with and without a postburst

increase; single-complex bursts with and without a postburst increase; gradual rises and falls of flux. In addition,

there is the designation "null* or no distinctive event. There

is strong evidence that there is an outstanding event or disturbance in 2800 Mc/sec radiation. One is a sudden bursttype feature which occurs during the rise to maximum of the

H 00 flare. The other is the more gradual rise and fall of

flux and "postburst increase," which lasts as long as, or longer than, the flare itself. Both types of phenomena appear to start the H CO flare. Flares associated with large

"postburst increases" or "gradual rises and falls" show a high concentration toward the central part of the solar disk.

This is not the cause for the strictly "burst -type" disturbances. The importance of the flare, the position of the

flare on the solar disk, and accompanying ionospheric disturbances are considered with respect to the form and energy

excess of the associated events at 2800 Mc/sec. (Met.

Abst. 6. 6-215. )--Authors' Abstract.

D-187 Dodson, H. W. (McMath-Hulbert Obs. , Univ. of Michigan),

Studies at the McMath-Hulbert Observatory of radio frequency radiation at the time of solar flares. Institute of Radio

Engineers, N. Y. , Proceedings, 46(1): 149- 159, Jan. 1958.

12 figs. , 4 tables, 11 refs. DLC--The complex flare phenomenon is described in terms of its photographic aspect of

Ha spectroheliograms, associated prominence activity, terrestrial effects, and the general pattern of radio frequency

emission. Flare-associated events at 2800 and 200 mc are

67
reviewed, and the association between flares and the on- set of 200 mc noise storms is discussed. Records of 2800

and 200 mc radiation at the time of 277 flares are compared.

Flare events at frequencies less than 200 mc are considered

and a study of 496 flares at 80 mc is summarized. An effort is made to compare reports of dynamic spectra at radio

frequencies with flare data and single frequency records.

The apparently close association between flares with "major

early bursts'" at frequencies ^200 mc and geomagnetic disturbances is discussed. (Met. Abst. 11. 5-157. )--Author's

abstract.

D-188 Dolbear, D. W. N. ; Elliot, H. and Dawton, D. I. , The cosmic ray intensity and radio fadeouts. Journal of Atmospheric and Terrestrial Physics, 1(3): 187-188, 1951. 6 refs.

MH-BH--The effect of small solar flares, causing short radio

fadeouts on cosmic ray intensity, was examined by superposing curves of cosmic radiation at Manchester before,

during and after 35 fadeouts between 9 h and 16 h S. M.T.

and 69 between 16 h and 9 h. Daytime results showed an

increase of cosmic rays by 0. 3% at time of fadeout; at night

this effect did not appear. (Met. Abst. 2. 9-95. )--C.E. P. B.

D-189 Douglas, J. N. ; Huguenin, G. R. and Lilley, A.E. , A very

low frequency radio experiment for satellite and probe trans - portation. Yale University. Observatory, Contract AF 19

(604) -3059, Final Report, Jan. 1960. 36 p. numerous figs,

(incl. photos), numerous tables, 3 refs. numerous eqs. -- The objectives of Contract AF 19(604)-3059 are: theoretical

and experimental investigations of the ionospheric regions

above the maximum of the F2 layer, by utilizing observations of extraterrestrial low frequency radio noise made in

rocket probes and satellites. The following sources of

VLF radiation are examined: general cosmic environment,

synchrotron radiation, plasma and shock waves, Cerenkov

radiation, parametric oscillations, free-free transitions,

solar disturbances, non-thermal planetary radiation, and

terrestrial disturbances. Based upon predicted VLF intensities to be expected from cosmic sources of radiation performance specifications on the antennae and radiometers

are developed. Three complete satellite payloads have

been constructed for rocket probe and satellite transportation. Each payload operates at 13. 25, 7. 0, 2. 2 and 0. 7

Mc. Ground based radiometers and ground based transmitters have been constructed for terrestrial correlation studies and "closed-loop" tests of ionospheric leakage. (Met.

Abst. 11. 12-583. ) --Authors' abstract.

68
D-190 Dowden, R.L. and Goldstone, G.T. (both, Commonwealth

Ionospheric Prediction Serv. , Hobart, Tasmania), "Whistler

mode" echoes remote from the conjugate point . Nature,

London, 183(4658): 385 -386, Feb. 7, 1959. fig., 3 refs.

,

2 eqs. DLC--An investigation, sponsored by the Australian

National Committee of the I. G. Y. has been made of the

Eckersley-Storey theory on whistler propagation. This

theory predicts that whistler mode signals from Tokyo (20

N geomagnetic latitude) would return to the Earth's surface

at a point near Darwin in the Northern Territory, some 3500

km from Hobart, Tasmania (51 S geomagnetic latitude).

Yet, when echoes of very low frequency radio signals were

established on 17. 44 kc/s in Tokyo with delays of approximately 0. 2 s, they were later detected at Hobart. It is

suspected that the echoes must have traveled via the whistler mode from Tokyo to the vicinity of Darwin and thence to

Hobart through the Earth-ionosphere wave guide mode. Details are discussed. (Met. Abst. 11. 12-327. )--N. N.

D-191 Drake, Frank D. and Ewen, H. I. , Broad band microwave

source comparison radiometer for advanced research in radio

astronomy. Institute of Radio Engineers, N. Y. , Proceedings, 46(l):53-60, Jan. 1958. 11 figs. , 13 refs. , 5 eqs.

DLC--A travelling wave tube radiometer operating at 8000

Mc with a bandwidth of 1000 Mc and sensitivities of the

order of 0. 01 K is described. The radiometer is more than

one order of magnitude more sensitive than other existing

radiometers operating at 8000 Mc. The very serious effects

of gain fluctuations, acting on small residual signals, when

trying to achieve very high sensitivities, are discussed. A

means of eliminating such effects by introducing compensating noise has been found successful. Radio observations

with this radiometer in conjunction with a 28 ft parabolic

reflector have shown that: (1) the predicted sensitivity is

achieved; (2) zero level stability is extremely high; (3)

it has been possible to detect in detail the distribution of

radio brightness at this wavelength in the vicinity of the

galactic plane; (4) radiation from the planets Jupiter and

Saturn has been detected, this being the first detection of

Saturn as a radio source; (5) radiation from two planetary

nebulas has been detected, this being the first detection

of these objects as radio sources. (Met. Abst. unpub. )--

Authors' abstract.

D-1S2 Drake, F. D. , How can we detect radio transmissions from

distant planetary systems? Sky and Telescope, 19(3):140-

143, 1959. 3 figs. DLC--A formula is given for distance

of detection of cosmic radio signals, by means of which it

is proven that our present radio equipment is capable of

69
receiving signals from other possibly existing civilizations

in space. Our search for radio contact with extraterrestrial

beings ought to be confined to between 1000 and 10, 000 Mc,

or rather at 1420 Mc, the frequency of the 21 cm interstellar hydrogen line, will prove satisfactory. --W. N.

D-193 Dueno, Braulio (Univ. of Puerto Rico, College of Agric.

and Mech. Arts, Mayaguez), Low angle fluctuations of the

radio star Cassiopeia as observed at Ithaca, N. Y. , and its

relation to the incidence of sporadic E. Journal of Geophysical Research, Wash., D.C., Sl(3):535-540, Sept. 1956.

4 figs. , 2 refs. DLC--Low angle fluctuation data of the ra- dio star Cassiopeia for the period comprised between Sept.

1954 to Aug. 1955, have been compared with ionospheric

sounder data from Ottawa, Canada. A remarkable relation

between the incidence of fluctuations and sporadic E has

been observed for the month of Dec. 1954. The coincidence

of Es and fluctuations were found, in general, to be very

good during the midwinter period and poor afterward. The

pierce-through region for ionospheric layers at a height of

400 km comes out approximately 1500 km north of Ithaca.

In this region the normal sun controlled forms of ionization

should be a minimum during the midwinter period. It is

reasonable to expect that layers at the 120 km level should

be most influential in causing fluctuations during this period. Several fluctuationless days were recorded during this

midwinter period and practically none at other times. (Met.

Abst. 9A-lll.)"Author's abstract.

D-194 Dumont, Rene, L' ionosphere et l'optique qeometrique des

ondes courtes . (The ionosphere and the geometric optics of

short waves.) Paris, Dunod, 1958. 100 p. 33 figs. , 11

refs. (Monographies Dunod, No. 3) DWB (M 10. 535

D893io), DLC (QC879. D85) Review in La Meteorologie,

Paris, Ser. 4, No. 49:75, Jan. /March 1958. --A pocketsize textbook giving basic and up-to-date information on

the ionosphere and its formation, structure, radio wave propagation, sounding by vertical pulses and by study of photo

chemistry, absorption, geomagnetic fluctuations, optical

phenomena, meteors and rockets. Characteristics of the

different layers, applications to long distance radio propagation, forecasting of ionospheric and radio propagation

conditions, etc. , are discussed. Aurora, airglow, sunspots, satellites, ionospheric tides and various theories

are treated incidentally. Numerous schematic diagrams, an

author and subject index are included. (Met. Abst. 10. 10-

17.)-M.R.

70
D-195 Dungey, J. W. (Sydney Univ. , School of Physics, N.S.W. X

Bailey's theory of sunspot noise. Journal of Atmospheric

and Terrestrial Physics, London, 4(4/5): 148-162, 1953. 10

refs. , 58 eqs. DWB-The exact formulation of BAILEY's

theory for a nonuniform ionized gas is described and the

boundary conditions are explained. A direct calculation is

made of the rate of exchange of energy between the motion

of the electrons and the wave. The intensity of the radiation arising from a transient disturbance is calculated and

it is found that the intensity can become very large when

the wave gains energy from the electrons. The general nature of the electron flow and the order of magnitude of the

electron velocity needed for amplification to occur are discussed. (Met. Abst. 9A-32.) --Author's abstract.

D-196 Dyce, R.B. (Stanford Res. Inst., Menlo Pk. , Calif.),

Faraday rotation observations of the electron content of the

exosphere (Summary only). Journal of Geophysical Research,

Wash., D.C., 65(9):2617-2618, Sept. 1960. table, 4 refs.

DLC--The polarization twist imposed on 106. 1 Mc/s radio

waves by the ionosphere has been investigated by using the

moon as a passive reflector. This has been done with a view of learning the total electron column density even at

altitudes above the known ionosphere. Because the antenna

is capable of being continuously directed at the moon for 12

consecutive hrs, observations are possible from the predawn

ionization minimum to the noontime maximum. (Met. Abst.

11. 12-438. )--Author's abstract.

D-197 Dyce, R.B. and Hill, R.A. (both, Stanford Res. Lab.,

Menlo Park, Calif. ), Lunar echoes received on spaced re - ceivers at 106. 1 Mc. Institute of Radio Engineers, N. Y.

,

Proceedings, 48(5):934-935, May 1960. fig., table, 9 refs.

DLC --Brief discussion of tests conducted at Stanford Research Institute in Jan. and April 1958, purporting to measure the sizes of the lunar patches and the possible speed

of motion of their reflected energy along the earth's surface.

Two interspaced antennas were directed at the moon at 15

min intervals, using precomputed values of azimuth and

elevation. The uncorrelated fluctuations (shown in graph)

imply that radio communication via the moon is possible

with a diversity distance of about 1 km at right angles to

the ray. (Met. Abst. unpub. )--W. N.

D-198 Easton, R.L. and Votaw, M.J. (both, U.S. Naval Res. Lab.,

Wash., D.C.), Vanguard I IGY satellite (1958 Beta). Review of Scientific Instruments, N. Y. , 30(2):70-75, Feb.

1959. 11 figs. , 2 tables, 3 refs. DWB, DLC--

71
The instrumentation used, the measurements obtained, and

the uses of the Vanguard I satellite are described. This

satellite contains two transmitters, one powered by batteries for about three weeks and one powered by solar cells

(still operating). From the transmitted frequencies temperature information and rotation rates are obtained. The transmitted signals are also used to determine the satellite orbit.

An approximate free orbital lifetime of 200 years is predicted. (Met. Abst. 10. 10-92. ) -Authors' abstract.

D-199 Ehmert, Alfred and Revellio, K. (both, Max-Planck Inst.

,

fur Physik der Stratosphare, Weissenau bei Ravensburg),

The influence of the solar eclipse of June 30, 1954 on lowfrequency atmospherics. (In: Solar eclipses and the ionosphere: a symposium. . . ed. by W. J. G. Beynon and G. M.

Brown. London, Pergamon, 1956. p. 126-131. 7 figs.

,

2 refs.) DWB--Records of atmospherics on 13 kc/s obtained

at Weissenau during the solar eclipse are compared with

other European records. For small atmospherics from distant centers, the variations show a distinct peak during the

eclipse. This peak is absent for stronger atmospherics of

the same frequency and also for higher frequencies from

nearer discharge centers. Narrow sector d. f. observations

at Payerne and Zurich, together with meteorological information, enable the source of these atmospherics to be located

near the Azov Sea and the Caucasus at distances from 2000

to 2500 km. Best transmission occurred when the sun was

more than 75% obscured at both reflection points for the

doubly reflected waves. (Met. Abst. 9. 6-291. )- -Authors'

abstract.

D-200 Ehmert, A. and Revellio, K. , Solare Ultrastrahlunq und

ionosph&ische D-Schicht am 23 Februaryl956. (Solar cosmic rays and the ionospheric D layer on Feb. 23, 1956.

)

Zeitschrift fur Geophysik, Wurzburg, 23(3): 113-134, 1957.

4 figs., 26 refs., eqs. DLC (QC801.Z4) -The outburst of

solar cosmic rays on Feb. 23, 1956, caused a strong attenuation of longwave atmospherics on the night side of the

earth. A discussion of our own and other records shows

that the beginning follows immediately the first arrival of

this solar radiation. The electron density caused by the

ionization of these cosmic rays is sufficient to cause the

observed attenuation. But this attenuation continued after

the decrease of cosmic ray intensity for several hours. It is suggested that negative ions formed by attachment of

electrons to 02 have a long life at night in low concentration and that at every time a small fraction of them is liberated for a short time. These electrons continue attenuation. (Met. Abst. 11F-35. )- -Authors' abstract.

72
D-201

D-202

D-203

D-204

Elgaroy, Oystein, Frequency drift of short-time transients

in solar radio noise . Nature, London, 180(4591): 862, Oct.

26, 1957. fig. , ref. DWB--Preliminary records on 199 and

200. 5 Mc/s at Oslo are analyzed and some conclusions

drawn. (Met. Abst. 9A-151. )--C. E. P. B.

ElgaroV, O. , Duration of transients in solar radio noise.

Nature, London, 180(4590):808-809, Oct. 19, 1957. fig.,

2 refs. DWB--Records of solar noise storms on 200 Mc/s

with a bandwidth of 0. 3 Mc/s show that bursts can be re- solved into several pips with a rather sharp peak at 0. 28

sec. They have a tendency to occur in groups; when wavelength is doubled mean duration is halved.

9A-150.)-C.E.P.B.

(Met. Abst.

Elgaroy, O. (Inst, of Theoretical Astrophysics, Univ. of

Oslo), Observations of the fine structure of enhanced solar

radio radiation with a narrow band spectrum analyser. Nature, London, 184(4690), Supp. No. 12:887-888, Sept.

19, 195S. 3 figs. , 3 refs. DWB--A narrow band swept re- ceiver was set up at Harestua to study the pips of enhanced

solar radio radiation. The operation of the receiver is ex- plained and the observations are described. On Aug. 18 a very remarkably fine structure was found in the 200 Mc/s

radiation. The observations of storm bursts are discussed

and shown in 3 photographs. (Met. Abst. 11. 12-49. )--I. S.

Ellis, G. R. A. , On the propagation of radio waves through

the upper ionosphere . Journal of Atmospheric and Terrestrial Physics, London, 9(l):51-55, July 1956. fig. , 2 tables,

7 refs. , 7 eqs. DWB--Since it is likely that electron densities of more than 0. 1 electron per cm^ exist at distances of

several thousand kilometers from the earth, the propagation

of the two low frequency extraordinary modes through the

ionosphere is improbable. Of the five possible ways in

which waves can penetrate the lower ionosphere, we therefore have only three which can also penetrate the upper ionosphere. Of these three, the oblique longitudinal ordinary

mode can produce only second order observational effects

in the absence of strong discrete sources of extra-terrestrial

radiation, since its angular range is only about 1 degree

(ELLIS, 1956). The low frequency limit for the observation

of cosmic radio emission will, therefore, in general be that

given by foF2, and the observation of these radiations from

below the ionosphere is unlikely at frequencies much less

than 1 Mc/s. (Met. Abst. 7. 11-158. ) --Author's abstract.

73
D-205 Ellis, G. R.A. (Radio Res. Labs., C.S. I. R. O. , Australia),

The trapping; of cosmic radio waves beneath the ionosphere.

Journal of Atmospheric and Terrestrial Physics, London,

13(1/2):61-71, Dec. 1958. 11 figs. , 5 refs. , 4 eqs. DLC

--The observation of cosmic radio noise at frequencies less

than the local ionospheric critical frequency is discussed.

It is shown that this effect may adequately be explained in

terms of the trapping of the radiation between the ionosphere

and the ground. Wherever there is a horizontal gradient of

critical frequency in an ionospheric layer, incoming extra

terrestrial radiation may be reflected by the layer after one

ground reflection and may subsequently propagate by hop

transmission for large horizontal distances beneath the layer.

A method of calculating the amplitude of the trapped radiation at any distance is given, allowing for all possible

modes. (Met. Abst. 10. 10-197. ) -Author's abstract.

D-206 Ellis, G. R. A. and Cartwright, D. G. (both. Commonwealth

Scien. & Indust. Res. Organiz. , New So. Wales), Directional observations of radio noise from the outer atmosphere.

Nature, London, 184(4395, Supp. No. 17): 1307-1308, Oct.

24, 1959. fig. , table. DWB--Observations made of the

radio emission of the Earth's outer atmosphere in the frequency band of 2-40 kc/s by a newly developed technique for

continuously monitoring the occurrence of such phenomena

are described. The bursts of low frequency noise have a

relatively narrow spectrum. Their likely mechanism is described. It appears possible to estimate the size of the virtual sources of very low frequency radiation. (Met. Abst.

11. 12-320. )--A.H.K.

D-207 Ellis, G. R.A. ; Cartwright, D. G. and Groves, J. R.V.

,

Spaced observations of radio noise from the outer atmosphere. Nature, London, 184(4696, Supp. No. 18) : 1391-

1392, Oct. 31, 1959. fig. , ref. DWB--It was suggested

by G. R. A.ELLIS in Planetary and Space Science that during

some types of radio noise storms in the Earth's outer atmosphere, the source of noise may remain in constant position

in right ascension. In this case the arrival of the storm

will be recorded at the same local time at places of different longitude rather than simultaneously. In a majority of

the cases noise bursts were recorded simultaneously at

Camden and Adelaid. A distinct time delay was observed

only during a major geomagnetic storm and aurora. (Met.

Abst. 11. 12-321. )-A. H. K.

74
during Sept. and Oc

from 135^ to 155°E,

D-208 Ellis, G. R.A. (C.S.I. R.O. , Camden, Australia), Directional observations of 5 kc/s radiation from the earth's

outer atmosphere. Journal of Geophysical Research, D. C.

,

65(3): 839-843, March 1960. 3 figs. , 2 tables, 5 refs.

DLC--Low frequency radio noise bursts associated with

geomagnetic disturbances have been observed with a network of direction finding receivers in southeastern Australia

and Oct. 1959. Over a range of longitudes

18 noise bursts came from apparent

sources at latitudes greater than 42 S. On 8 occasions,

isolated, discrete noise sources with an average geographical size of 550 km were detected at latitudes between 34 S

and 42°S. (Met. Abst. 11. 12-322. ) -Author's abstract.

D-209 Ellis, G. R.A. (C.S.I. R.O. , Australia), Geomagnetic

disturbances and 5 kilocycles per second electromagnetic

radiation. Journal of Geophysical Research, Wash. , D. C.

,

65(6): 1705-1710, June 1960. 6 figs. , 12 refs. DLC--

A comparison is made between variations of the geomagnetic field and bursts of 5 kc/s radio noise recorded at

Camden, N.S.W. , between June 1958 and Oct. 1959. During this period 8 noise storms were recorded. All occurred

during the main phase of a geomagnetic storm, beginning

on the average 3 hours after the start of the main phase.

Of 97 isolated noise bursts of less than 4 hours' duration,

43 were associated with positive bays in the record of the

magnetic H component. No consistent delay between the

noise burst and the bay was observed. Noise bursts were

net in general associated with geomagnetic micropulsations of less than 1 minute period, although some correlation with quasi-sinusoidal magnetic variations with periods

between 10 and 60 minutes was noted. During the period

of the observations 30 magnetic sudden commencements

were followed by noise bursts or storms after an average

delay of 8. 5 hours. On four occasions, a noise burst

started immediately after a sudden commencement occurring

between 1200 and 1800 hrs GMT. (Met. Abst. 11. 12-310. ) --Author's abstract.

D-210 Ellison, Mervyn Archdall, Source points of radio noise

bursts associated with solar flares. Nature, London,

167(4258):941-942, June 9, 1951. 12 refs. DLC--Discussion of a number of recent observations of visible flares

followed after a lag by radio noises, and their meaning in

solar physics. Author discusses exact relation between

visible radiation from flares and radio noise apparently

from the same source point. (Met. Abst. 3.3-141.)—

C.E.P.B.

75
D-211 Ellison, M.A. (Royal Obs. , Edinburgh), The H Eradia- tion from solar flares in relation to sudden enhancements

of atmospherics on frequencies near 27 Kc/s . Journal of

Atmospheric and Terrestrial Physics, London, 4(4/5):226-

239, 1953. 5 figs., 2 tables, 18 refs. DWB--The development curves of 10 solar flares observed in H to light are compared with the sudden enhancements of atmospherics

(S.E. A. s) generated by them. In confirmation of earlier

work (1950), an average time lag of 7 min is established

between the maximum of the flare and the maximum of the

resulting S.E. A. This is interpreted as an effect of "sluggishness* in the response of the D layer (at a height of

about 75 km) to the ionizing radiation from the flare. An

analysis is made of the association of S.E. A. s with 413

flares of Classes 1, 2 and 3 during a period of 4 years.

In the hours between 0900 and sunset 51% of Class 1 flares,

88% of Class 2 flares and all Class 3 flares have associated

S.E. A. s. The percentage association is higher during the

middle of the day and in the afternoon than in the early morning hours. It is also higher in winter than in summer. It is emphasized that three or four 27 kc/s recorders well distributed in longitude would give almost complete coverage

for the recording of major flares; the method might profitably be used during the International Geophysical Year of

1957. (Met. Abst. 7. 4-133. )--Author's abstract.

D-212 Ellison, M.A. (Royal Obs. , Edinburgh), The sun and its

influence: an introduction to the study of solar-terrestrial

relations. London, Routledge and Kegan Paul, 1955. 235 p.

54 figs. , 9 plates, 9 tables, bibliog. p. 225-230. Price:

21 sh. DLC (QB531.E4 1955). Review by J. Pepper in

Royal Meteorological Society, Quarterly Journal, 82(354):

549-550, Oct. 1956. Review by F. Steinhauser in Archiv

fur Meteorologie, Geophysik und Bioklimatologie, Ser. A,

9(3):428-430, 1956. DLC -The latest discoveries in var- ious fields of astro- and geophysics connected with solar

terrestrial relationships (not including solar-weather relations) are woven into this systematic yet readable book on

the sun, its radiations, atmosphere, disturbances, etc.

,

and their effects on cosmic ray, geomagnetic, ionospheric,

and auroral and radio phenomena or disturbances. Many

excellent schematic drawings, photos and tables are included. (Met. Abst. 8. 7-6. )--M.R.

D-213 Ellison, M.A. (Royal Obs. , Edinburgh), Solar flares.

(In: Beer, Arthur (ed. ), Vistas in astronomy, pub. London,

1955-56. Vol. 2:799-807. 4 figs. , 14 refs.) DLC, DWB

(520. 82 B415v)--A review of the progress during the past

25 yrs. and present knowledge of solar flares and their

76
relation to sudden disturbances in the ionosphere, fadeouts, radio noise, etc. General properties of solar flares,

flare spectra, ionospheric effects and radio emission are discussed at some length and recent theoretical work re- viewed. (Met. Abst. llD-37.)--M.R.

D-214 Ellison, M.A. (Royal Obs. , Edinburgh), Sudden ionospheric disturbances in relation to solar flare radiations . (In: Solar eclipses and the ionosphere: a symposium. . . ed.

by W. J. G. Beynon and G. M. Brown, London, Pergamon, 1956.

p. 180-183. 6 refs.) DWB--A solar flare emits a burst of

ultraviolet radiation which has immediate repercussions in

the D and lower E regions. The operative wavelengths are

still uncertain; but L OP (1216 A) radiation at the higher

levels and X-rays (^5 A) at lower levels seem probable.

Comparisons have been made between the development

curves of the S. I. D. 's and of the H (36 radiation of the

flares which caused them. On the assumption that the

ultraviolet follows the same variation with times as the

H 06 light, some deductions can be made about the relaxation times and the maximum ionization at various levels.

(Met. Abst. 9. 1-175. ) -Author's abstract.

D-215 Ellison, M.A. (Prof. Astronomy, Dublin Inst, for Advanced Studies), The sun and its influence: .an introduction to

the study of solar-terrestrial relations . 2d ed. rev. London,

Routledge and Kegan Paul, 1959. 237 p. figs. , tables,

foot -refs., bibliog. p. 227-232. DWB (523. 7 E47s). Review by C. W.Allen in Nature, London, 186(4718):69, April

2, 1960. -The first (1955) edition of this small book has

been slightly revised and updated to include preliminary

material on the subject of solar-terrestrial relations emanating from the IGY. The subjects treated in a readable

manner are: solar radiation, solar activity, solar atmosphere, ionosphere, solar flares and their effects on the

earth's atmosphere, effects on geomagnetism, the aurora,

radio waves from the sun and, finally, cosmic rays. Appended are tables or theory for finding mass of the sun,

radiation laws and sun temperature, Zurich sunspot numbers for 200 yrs, radio flux from sun and radio propagation

in ionosphere and corona. Extensive references arranged

by chapters are also appended. (Met. Abst. 11.9-6.) —

M.R.

D-216 Elsasser, H. , Die Szintillation der Sterne. (The twinkling of stars.) Die Naturwissenschaften, Berlin, 47(1):6-10,

Jan. 15, 1960. 9 figs. , table, 18 refs. DLC -General sur- vey and discussion of the results obtained during the last

years in the study of the twinkling of stars: methods of

measurement and reduction; use of the secondary electron

77
multiplier; no agreement concerning the determination of

the magnitudes; brightness twinkling: good frequency

spectra obtained until 0. 1 Hz, but uncertain and disturbed

below 0. 1 Hz; dependence on the aperture of telescope,

the zenith distance and the altitude above sea level from

where observations are done. On the Jungfraujoch the

deviation or reaches only 55% of the & measured at sea

level. Interesting information on the directional twinkling

as a function of zenith distance was obtained. Discussion

of a correlation between brightness and directional twinkling and of Hosfeld's experiment; twinkling and wind speed:

Mikesell's diagram, brightness changes for various frequencies and wind force. Correlation is sometimes possible.

Discussion of the results obtained at the Boyden Station

(March-Sept. 1956) with Danjon's visual method. Author

takes into account the influence of the whole atmosphere.

The deviation of the refractive index from the mean value

reaches 10-8 while the temperature variations reach 10"^

degree. The lower layers of the atmosphere exert the

strongest influence on the directional twinkling, whereas

brightness is influenced by the part of the atmosphere comprised between 8 and 12 km. (Met. Abst. 11.8-55.) —

A.V.

D-217 Erickson, W. C. (Convair Scientific Res. Lab., San Diego,

Calif. ), Observations of 26.3 Mc/s solar radio noise during Aug. 1959. Journal of Geophysical Research, Wash.

,

D.C., 66(6): 1773- 1780, June 1961. 3 figs. , 8 refs. DLC

--Decameter wavelength observations of the solar noise

storm during the latter portion of Aug. 1959 were obtained

at this laboratory. These data displayed several characteristics not apparent in the observations at shorter wavelengths. First, we observed decameter wavelength emission before the meter Wavelength emission was observed.

Second, intense decameter wave emission ended on Aug.

25, whereas intense meter wavelength emission persisted

until Sept. 3. Third, our observations indicate quite uniform emission. We did not observe the intense amplitude

scintillations found by other observers. Our observations

tend to confirm the identification of this disturbance as a type I noise storm. Even at decameter wavelengths, the

emission region appeared to be of small angular diameter,

and low in the corona. --Author's abstract.

D-218 Evans, John W. (Upper Air Res. Obs. , Sunspot, N. Mex. ),

Solar influence on the earth. Smithsonian Institution, Wash.,

D.C., Annual Report, 1954, pub. 1955. p. 189-200. DWB,

DLC --The author has given a broad general coverage of the

entire field of solar-terrestrial-ionospheric-magnetic relationships in this James Arthur lecture given under the

78
auspices of the Smithsonian Institution on May 27, 1954.

Models and effects are described and illustrated by homely

and sometimes humorous analogies. The different kinds of

radiation reaching the earth from the quiet and disturbed

sun are emphasized and their effects on ionosphere-atmosphere and radio touched upon. The purpose of the new Air

Force Cambridge Research Center Observatory at Sunspot,

N. Mex. , on Sacramento Peak at 9000 ft is stated to be

merely to learn more about the sun. (Met. Abst. 8. 4-317. ) -M.R.

D-219 Fan, C.Y. ; Meyer, P. and Simpson, J. A. (all, Univ.

Chicago), Preliminary results from the space probe Pioneer

Vi Journal of Geophysical Research, Wash., D.C.,65(6):

1862-1863, June 1960. 2 figs., 2 refs. DLC--Solar flare

particles producing ionization in the polar atmosphere for

many hours are not stored in the geomagnetic field. Evidence has been found for the solar production of energetic

electrons by processes other than solar flares. Bremsstrahlung was measured in Pioneer V. (Met. Abst. 11. 12-

99.)--E.Z.S.

D-220 Faust, H. , Importance of artificial satellites for meteor*

oloav. Universitas, Stuttgart, 2(l):93-94, 1958. DWB--

Density, temperature, and composition of the rare atmosphere at 200-300 mi are among the important information

that can be gained better from a satellite slowly spiraling

toward the earth than from one entirely outside the earth's

atmosphere. Incident and reflected radiation, UV and cosmic rays during solar eruptions, effect of ozone layer, and

other data which will materially aid in short and even in

long range weather forecasting will be provided by a ser- ies of satellites whose economic benefits will far outweigh

the cost, high though this is. (Met. Abst. 10.7-91.)--

M.R.

D-221 Feins tein, Joseph, Some stochastic problems in wave pro- pagation, Pt. 1. Institute of Radio Engineers, Professional

Group on Antennas and Propagation, Transactions, Vol.

AP2(l):23-30, Jan. 1954. 5 refs. , 43 eqs. DLC--The effect of random height variations associated with a conducting surface upon the characteristics of reflected wave

energy is ascertained by the methods of physical optics.

Average received power, its variance, angular and frequency power spectra, and the field correlation pattern are determined in terms of the statistical parameters of the

surface. Volume type problems are treated by ascertaining the effect of refractive index fluctuations within a slab

upon an emergent wave front, and then generalizing to a

79
continuous medium. The results are applied to various

problems encountered in tropospheric and ionospheric

wave propagation. --Author's abstract.

D-222 Fensler, W.E. ; Senior, T.B. A. and Siegel, K.M. (all,

Michigan Univ. ), Exploring the depth of the surface layer

of the Moon from a radar space observatory. Aero/Space

Engineering, N. Y. , 18(11):38-41, Nov. 1959. 4 refs. , 5

eqs. DLC--The method given here involves the determination of the power reflection coefficient at different wavelengths; this coefficient is a function of the number and

depth of any layers present and of the electromagnetic constants associated with these layers. Using the mathematical formula for the reflection coefficient of a layered structure, these quantities can be calculated from measured

values of the power return at different wavelengths. It is

suggested that this experiment be carried out by placing a radar-equipped satellite in orbit around the Moon; data on

the power reflection coefficient could be telemetered back

to earth for analysis. The feasibility of the whole system

is discussed. (Met. Abst. 11. 12-180. )--Authors" abstract.

D-223 Ferraro, V.C.A. , Geophysical aspects of solar flares . Nature, London, 175(4449):242-244, Feb. 5, 1955. DWB--

Summary of Geophysical Discussion at Royal Astronomical

Society on Nov. 26, 1S54. H. W. NEWTON described effects of solar electromagnetic and particle radiation. J. S.

HEY described distribution of solar flares across disc with

associated radio bursts on 4. 1 m. M. A ELLISON dealt

with the flash of UV radiation generated by a flare and sudden ionosphere disturbances. He attributed crochet cur- rents to increased conductivity and an independent current

system at base of D layer, about 60-70 km. Kn WEEKES

discussed distribution of extra ionization during a solar

flare, finding the greater part in 95-100 km with independent ionization near 70 km. H.ELLIOTT discussed increases

of cosmic rays during intense solar flares. (Met. Abst.

6. 7-27.

)

D-224 Fetner, E. M. (RCA), Shock-layer attenuation data collect- ed from missile tests at the Atlantic missile range. Planetary and Space Science, N. Y. , 5:225, June 1961. Abstract

only. The paper was presented at the Plasma Sheat Symposium, Boston, Mass. , Dec. 7-9, 1959. --The problem of

propagating electromagnetic energy through shock layer

ionization has been a concern of theorists for the past

several years. Theory on the subject has been fairly well

explored. Also, some experimental data have come from

laboratory shock tube tests. However, not until recently

has this re-entry phenomenon been actually observed.

80
D-225

D-226

D-227

During the past year data at telemetry and S-band frequencies from several IRBM and ICBM tests have been collected. Samples of these data and other related information,

such as velocity and altitude, are presented.

Fleming, John Adam (ed. ), Terrestrial magnetism and

electricity. Contributors, J. Bartels and others. (Reprinted

with corrections.) N. Y. , Dover Publications, (1949). numerous figs., tables, eqs. (Physics of the Earth, v. 8).

DLC--An excellent reference work on all aspects of the subject. It contains 12 chapters written by experts in the

field, and a comprehensive bibliography of 1523 refs. in

ch. 13 . Three chapters particularly applicable to this bibliography are: ch. 9, Berkner, L.V., Radio exploration of

the earth's outer atmosphere (p. 439-491). Ch. 10, Hulburt, E. O. , The upper atmosphere (p. 492-572). Ch. 13,

Harradon, Harry Durward, Bibliographic notes and selected

references (p. 679-778). Section D of the bibliography

(p. 749-758) contains 183 references to works on the ionosphere,. The bulk of the material was published in the 1920's

and 1930's. (Met. Abst. 6D-30. )-M.L. R.

Fokker, A. D. ; de Munck, J. C. and de Feiter, L. D. (all,

Netherlands Postal and Telecommunications Services, The

Hague), Eclipse observations of solar radio-frequency

radiation on 200, 545, 3000, and 9100 Mc/s . (In: Solar

eclipses and the ionosphere: a symposium. . . ed. by W. J. G.

Beynon and G. M. Brown. London, Pergamon, 1956. p. 272-

274. fig.) DWB--A brief summary is presented of solar

radio noise observations on four frequencies during the

eclipse of June 30, 1954. In the case of the frequencies

545 and 200 Mc/s, the duration of the radio eclipse ex- ceeded that of the optical eclipses by about 10 and 13 min.,

respectively. For the higher frequencies the durations of

the radio and optical eclipses are approximately equal. In

most cases, maximum phase of the radio eclipse occurred

some minutes later than that of the visual eclipse. (Met.

Abst. 9A-162. )--Authors' abstract.

Fokker, A. D. , Een zeldzaam radiofenomeen op de zon. (An unusual solar radio phenomenon. ) Hemel en Darnpkring. The Hague, 56(6):115-116, June 1958. fig. DWB,

DLC--On Nov. 4, 1957, an unusual solar burst was observed at Nederhorst den Berg (Netherlands) at 8.48 U.T.

The solar radio noise on 200 M Hz increased strongly:

after 40 minutes the intensity was 1000 times higher than

normal and it continued to increase for 5 hours. No "Dellinger effect" was noted and the increasing radio radiation

presented very characteristic intensity oscillations. From

81
the recordings on 4 - 11 - 57, it was stated that the intensity fluctuations had a completely different character than

usually recorded from the sun. The author gives a photo

of the recording. --A. V.

D-228 Fokker, A. D. , Ruis-actieve gebieden op de zon. (Regions

of noise activity on the sun. ) Hemel en Dampkring, The

Hague, 57(6):139-151f June 1959. 12 figs. DWBf DLC--

The radio emission on meter wave lengths, with irregularly

varying intensity is discussed. The article is greatly

based on the radio astronomy observations carried out during recent years at the P.T.T. radio receiving station NERA

at Nederhorst den Berg (Netherlands). A description is

given of the interferometer used, receiving on 1. 18 m wave

length. A study is made of the effect of sunspots on radio

storms; the measurement of the polarization of radio emission (linear or elliptic) and the role of magnetic fields in

the corona on the circular polarized radio emission. Figures are presented of recordings of radio emission and of

clockwise, counterclockwise, and mixed polarization with

the corresponding interferometer positions. (Met. Abst.

11.8-79.)--A.V.

D-229 Forbush, S. E. and Burke, B. F. (both, Dept. of Terrestrial

Magnetism, Carnegie Institution of Washington), Absorp- tion of cosmic radio noise at 22. 2 Mc/sec following solar

flare of Feb. 23, 1956. Journal of Geophysical Research,

Wash., D.C., 61(3):573-575, Sept. 1956. fig., 2 footrefs. DLC--A phase switching interferometer measured the

absorption at 22. 2 Mc/s from the radio source Virga A.

The intensity on Feb. 23, 1956 at 0430 GMT was less than

0. 1 the intensity on Feb. 22, 1956. Cosmic ray intensity

showed similar effects. The measurements were made near

Washington, D.C. Comparison with other type of measurements suggests the absorbing material for 22. 2 Mc/s was

above the F2 layer and may have been in the form of a localized cloud. (Met. Abst. 12.6-172.)-

D-230 Forsyth, P. A. and Paulson, K.V. (both, Univ. of Saskatchewan, Saskatoon, Sask. ), Radio star scintillations and

the auroral zone . Canadian Journal of Physics, Ottawa,

39(4):502-509, April 1961. 4 figs. , 13 refs. DWB, DLC--

A continuous series of observations of scintillations of the

radio star, Cassiopeia A, carried out at Saskatoon at a frequency near 53 Mc/s over a period of nearly 4 yrs has

been analyzed. The altitude angle dependence of the scintillations was very strong in 1955 but weak in 1958. This

behavior suggests that the scintillations are not produced

in a uniform layer of the atmosphere. It seems more likely

82
that the scintillations arise most strongly in regions of the

atmosphere closely associated with the auroral zone and

that these regions migrate southward during years of intense

sunspot activity.

D-231 Fricker, S.J. ; Ingalls, R.P. ; Mason, W. C. et al. , Computation and measurement of the fading rate of moon reflected UHF signals. U.S. National Bureau of Standards, Journal of Research, Sec. Df 64(5):455-465f Sept. /Oct. 1960.

11 figs., table, 8 refs. , 41 eqs. DWB, DLC--A method is

described for predicting the fast fading rate of moon reflected signals. It is based entirely upon considerations of the

observer-moon positions and relative motions. Experimental results which are in good agreement with the computed

fading rates have been obtained from a moon-reflection ex- periment at a frequency of 412 Mc/s. Some possible implications of this method of interpreting fading rates are given. (Met. Abst. 11L -124. ) --Authors' abstract.

D-232 Friedman, H. and Chubb, T. A. , Solar X-ray emission and

the height of the D layer during radio fade-out. (In: Physical Society of London, Physics of the ionosphere. London,

1955. p. 58-62.) table, 14 refs. DWB (M10. 535 C748)-

Rocket measurements show that Lyman alpha radiation of

hydrogen is the major source of ionization in normal D layer

and that solar X-rays contribute to the uppermost portions.

Evidence exists that X-rays as short as 1-2 A, together

with enhanced Lyman alpha radiation, are generated during

a solar flare. The largest flares are accompanied by sudden phase anomalies which indicate a lowering of the re- flecting ceiling for long waves by as much as 15 km. To

produce the necessary ionization at the lower levels, L X

intensity would need to increase by 10^* during the flare,

3 -2 -1 reaching a peak value of 10 erg cm sec . An X-ray

-5 -2 -1

flux of only 10 erg cm sec would form the required re- flecting layer at 60 km. (Met. Abst. 12. 1-116. ) -Authors'

abstract.

D-233 Frihagen, J. and Troim, J. (both, Norwegian Defence Res.

Estab. ), Scintillations of the 20 Mc/s signal from the

earth satellite 1958 S II. Journal of Atmospheric and Terrestrial Physics, London, 18(l):75-78, April 1960. 3 figs.

DLC--This note gives some preliminary results which have

been obtained at Kjeller, 60° N 11° E, in connection with

a study of scintillations of the signals from the earth satellite 1958 8 II. It is well known that studies of the movements and structure of the diffraction pattern formed over

the ground by radio signals either reflected from or transmitted through the ionosphere, may give information about

83
the structure and movements of the irregularities of the

electron density in the ionospheric layers. However, when

use is made of the signals transmitted from a satellite like

1958 6 II, which itself moves with a velocity far greater

than the velocity of the ionospheric irregularities, an amplitude pattern is produced over the ground which moves

with a velocity determined by: (i) the velocity of the satellite and (ii) the height of the irregularities producing the

scintillations as compared with the height of the satellite.

It would, therefore, seem possible to obtain information on

the height of the irregularities from observations of scintillations of satellite signals. The discussion in this note is

divided between the scintillations which are produced in

the F region and those which are produced in the E region.

Only 20 Mc/s recordings have so far been made. (Met.

Abst. 11.12-367. )--Authors' introduction.

D-234 Fuster, Arsenio, Influencia planetaria en la percepcion

de la radiacion. (Planetary influence in the perception of

radiation.) Las Ciencias, Madrid, 19(4):834-840, Oct./

Dec. 1954. 5 figs. DLC--An attempt to determine roughly

the effect of the incidence of sunspots, eclipses, planetary configurations, etc. , on ionospheric or radio propagation phenomena, based on 1946, 1947, and 1948 data, and

to explain effects with aid of schematic diagrams. (Met.

Abst. 6.8-144.)-M.R.

D-235 Gallet, Roger M. (Nat'l. Bur. Standards, Boulder, Colo.),

Aerodynamical mechanisms producing electronic density

fluctuations in turbulent ionized layers . Institute of Radio

Engineers, N. Y. , Proceedings, 43(10): 1240-1252, Oct.

1955. 8 figs. , table, 7 foot-refs. , bibliog. p. 1252, numerous eqs. DLC --Various radio effects of the turbulence in

the low ionosphere are discussed with a view toward determining the order of magnitude of the turbulence parameters

in this region. These effects include vhf scattering, sporadic E layer phenomena, and diffraction patterns in reflection. The required electron density fluctuations ( A. N N)

fluctuate around 10"4 and the scale of the turbulence Z is

roughly 100 to 200 m. The latter quantity measured directly

in the troposphere is of about the same order of magnitude.

The underlying purpose of the paper is to study the aerodynamical mechanisms of turbulence. Pressure fluctuations

result from the "collisions and extensions between turbulent

eddies" in a uniform gas, or from vertical transport in the

atmosphere with its varying pressure. It is shown that such

pressure fluctuations are too small, by a factor of about

10"4, to produce the observed density fluctuations. However, the vertical transport mechanism produces two other

84
effects which are independent of the energy of the turbulence and are of the right order of intensity. First, in a nonadiabatic atmosphere the vertical transport of air masses produces fluctuations of temperature. These, in turn,

give rise to air density fluctuations, and proportional electron density fluctuations. Second, fluctuations of electron

density result directly from transport in the presence of a gradient of electron density. These two effects, for the

same uniform turbulence, occur at different levels in an

ionospheric layer. They are sufficient to explain the

stratification properties of sporadic E. An expression for

the scale of turbulence is obtained from the gradients of

winds circulating in the low ionosphere. Hence, the properties of sporadic E phenomena should be interpreted in

terms of meteorological factors (winds, synoptic masses

of air, fronts, etc.). It is pointed out that the same transport mechanisms are acting in the troposphere, the gradients of water vapor content playing the role of the gradients of electron density. (Met. Abst. 7.8-262.)--

Author's abstract.

D-236 Gallet, R.M., The very low frequency emissions gen- erated in the earth's exosphere . Institute of Radio Engineers, N.Y. , Proceedings, 47(2):211-231, Feb. 1959. 15

figs. , '2 tables, 13 refs. , 14 eqs. DLC --Naturally occurring, very low frequency signals not associated with lightning discharges, and strongly correlated with solar activity,

have been recognized nearly as long as the atmospheric

whistlers which have their genesis in lightning discharges.

Whereas whistlers have been satisfactorily explained, until recently these other phenomena have not. From the ex- amination of a large quantity of high resolution spectrograms, it has been deduced that a major fraction, if not

all, of the other "noises" are excited in the exosphere by

streams and bunches of high speed ionized particles precipitating into the ionized atmosphere in the presence of

the earth's magnetic field. The electromagnetic waves

excited are then propagated in the manner of whistlers. The

excitation mechanism is similar to the operation of a travelling wave tube. Two frequencies are simultaneously generated, and are given by:

cd ^K"&-?;}*]•

Their values depend only on the three parameters: local

electronic density in the exosphere, local magnetic field

intensity, and particle velocity V. For a large range of

85
conditions, corresponding to middle latitude observations,

the low frequency explains many types of noise, and re-

•> fr) duces to ~WH" * Most of the observations require particle velocities of the order of 10, 000 km/

sec. The shape of the spectrum is also very sensitive to

the ambient electronic density distribution. A model in

which the ratio of electron density to magnetic field strength

is almost constant, along a line force in most of the exosphere, seems indicated by several types of noise. Such a

model satisfies also the whistler data. The problem of the

production of bunches and streams or particles is briefly

discussed. (Met. Abst. 11. 10-221. )--Author's abstract.

D-237 Gallet, R.M. and Helliwell, R.A. , Origin of " very-lowfrequency emissions.

U.S. National Bureau of Standards,

Journal of Research, Sec. D, 63(1) .-21-27, July/Aug. 1959.

4 figs., 2 tables, 14 refs. , 9 eqs. DLC, DWB--Selective

traveling wave amplification in the outer ionosphere is

postulated to explain very-low-frequency emissions, a class

of very low frequency (1 to 30 kc/s) natural noise. By analogy with the mechanism of traveling wave tubes, low level

ambient noise in the outer ionosphere is amplified in streams

of incoming ionized solar particles at frequencies for which

the stream and wave velocities are equal. Required velocities are in the range 0. 01 to 0. 1 c (where c is the velocity

of light). Streams with densities of the order of one electron per cubic centimeter would provide sufficient energy.

Phenomena which can be explained qualitatively by the

theory are the hiss, quasi-constant tones, dawn chorus and

related transients, and very long trains of whistler echoes.

A quantitative example shows how the theory can reproduce

the general form of certain characteristic discrete spectra

"hooks" of emissions, and how this leads to definite values

of particle velocity and a law for the distribution of electron

density in the outer ionosphere. (Met. Abst. 11F-45. )--

Authors' abstract.

D-238 Gallet, R.M. and Utlaut, W. F. (both, Nat'l. Bur. of

Standards, Boulder, Colo. ), Evidence on the laminar nature

of the exosphere by means of guided high frequency wave

propagation. Physical Review Letters, N. Y. , 6(11):591-

594, June 1, 1961. fig., table, 16 refs. DLC -Results of a series of experiments are reported concerning the laminar

structure of the exosphere for testing the existence and properties of the sheets at large distances, with the suggestion

to use this method for the determination of the permanent

ring current, observed in Explorer VI and Pioneer V

86
measurements. Experiments were conducted from late

April to June 1960 to observe the signal propagation and

backscattering from the ground at the point in the other

hemisphere which is the magnetic conjugate of the transmitter. Table shows the summary of one set of data.

(Met. Abst. unpub. )--E. K.

D-239 Garriott, Owen K. (Stanford* Univ. ) f The determination of

ionospheric electron content and distribution from satellite

observations, Pt. I, Theory of the analysis. Journal of

Geophysical Research, Wash., D.C., 65(4): 1139-1150,

April 1960. 9 figs. , 11 refs. , 31 eqs. Pt. 2. Results of

the analysis. Ibid. p. 1151-1157. 7 figs. , 9 refs. , 10

eqs. DLC. Also issued in International Geophysical Year

1957/1958. IGY World Data Center A (for) Rockets and

Satellites (National Academy of Sciences, Wash., D.C.),

IGY Satellite Report Series, No. 10, Jan. 1960. 65 p. 23

figs., 21 refs., 58 eqs. DWB (621. 1388 161s a) -The re- sults of observations of the radio transmissions from Sputnik III (1958 6 2) in an 8 month period, are presented. The

measurements of integrated electron density are made in

two ways, described in part 1. The measurements reveal

the diurnal variation of the total ionospheric electron content; also the ratio of the total content to the content of

the lower ionosphere below the height of maximum density

in the F layer is obtained. An estimate of the average

electron density profile above the F layer peak is made

possible by the slow variation in the height of the satellite due to rotation of the perigee position. The gross effects of large magnetic storms on the electron content and

distributions are found. (Met. Abst. 11. 12-368. )--

Author's abstract.

D-240 Garriott, O.K. and Little, C.G. (Nat'l. Bur. of Standards,

Boulder, Colo.), The use of geostationary satellites for

the study of ionospheric electron content and ionospheric

radio wave propagation . Journal of Geophysical Research,

Wash. , D.C., 65(7) :2025-2027, July 1960. 9 refs. DLC--

This paper describes a proposed radio propagation experiment utilizing a geostationary satellite. The experimental

methods for determining the total electron content of the

ionosphere are discussed, and the advantages and capabilities of the methods are summarized. Other possible studies utilizing the satellite transmissions are also outlined.

(Met. Abst! 11. 12-369. )--Authors' abstract.

87
D-241 Gates, David M. , Preliminary results of the National

Bureau of Standards radio and ionospheric observations

during the International Geophysical Year. U.S. National

Bureau of Standards, Journal of Research, Sec. D, 83(1):

1-14, July/Aug. 1959. 11 figs. , 2 tables, 18 refs. Also

shorter version issued as NBS radio, ionosphere, and airglow observations during IGY, in American Geophysical

Union, Transactions, 40(4): 391 -401, Dec. 1959. 8 figs.

DLC, DWB--A review is given of the activities of the National Bureau of Standards during the IGY. The equipment

used on each project is described and preliminary results

of the observations are given. The following areas of re- search are discussed: (1) World Warning Agency, (2)

Ionospheric Vertical Sounding Stations, (3) VHF Propagation, (4) VHF Equatorial Forward Scatter, (5) Radio Noise

Network, (6) Radio Satellite Observations, (7) Airglow

Observations, and (8) World Data Center for Airglow and

Ionosphere. (Met. Abst. 11E-53. )--Author's abstract.

D-242 Gendrin, Roger, Generation de bruits tres basse frequence dans 1' exosphere par effet Cerenkov. (Very low frequency noise generated in the exosphere by Cerenkov

effect. ) Academie des Sciences, Paris, Comptes Rendus,

251(10):1122-1123, Sept. 5, I960, fig., 8 refs. DWB,

DLC --The path travelled by the energy of a very low frequency wave can be directed along the magnetic field Ho;

either when the normal to the wave is directed itself along

Ho, or when the angle agrees with the relation Cos = 2 x where is the angle to the magnetic field of the normal

on the wave, and x the variable denoting the frequency of

the electromagnetic wave. The Cerenkov effect, caused

by relatively slow particles (10, 000 km/s) from solar origin, is capable of emitting selectively each frequency

under the angle complying with the relation Cos s 2 x. The total energy propagates then in the second mode. At

the same time the particle emits all the frequencies. Those

propagating at the same speed and following the same path

cause a noise of mostly constant amplitude in a large frequency band as long as the interaction between the particles and the exosphere continues. --A. V.

o43 Gerson, Nathaniel C. (Geophysical Res. Dir. , Cambr. , Mass.), A note on the conference on ionospheric physics.

U. S. Air Force. Cambridge Research Center, Geophysics

Research Papers, No. 11:13-14, 1952. DWB--The author,

in his introductory remarks to the conference reports, brings

out the fact that physicists have neglected many important

fields of research, such as were represented in this conference (physics of the high atmosphere and study of planetary atmosphere) while concentrating on nuclear and cosmic

88
D-244

D-245

ray research. The atmosphere is considered as comprising

several shells; the ionosphere (80-400 km), the mesosphere

(400-1000 km) and the exosphere (above 1000 km). Specific problems which are being solved are: dissociation and

recombination processes, correlation of solar and ionospheric phenomena, improvement of spectroscopic methods

and microwave observational techniques. (Met. Abst.

4. 10-107. )-M.R.

Gerson, N. C. (Arctic Comm. U.S.Nat'l. Comm. IGY),

Periodicities in solar radio noise emission. Australian

Journal of Physics, Melbourne, 12(3): 299-300, Sept. 1959.

fig., table, 4 refs. DLC--A note indicating the presence

of sweeper trains in the work of ROBERTS (1958) in which

he described solar radio wave emissions in the range 40-

80 Mc/s. In a reproduction of his Figure I the elements

of several sweeper trains (A-E) are indicated. Periods of

the trains are tabulated. (Met. Abst. 11. 12-51. )--I. S.

Gerson, N. C. (Arctic Committee, USNC for IGY) and

Gossard, W. H. (U. S. Dept. of Defence), Sweepers . Journal of Atmospheric and Terrestrial Physics, London,

17(l/2):82-85, Dec. 1959. 2 figs. , table, eq. Comment

by J. M. Watts, Ibid., 18(1):81, April 1960. DWB, DLC--

In studying whistlers recorded at Palo Alto, Calif, it was

found that most atmospherics in the hf band sweep through

a finite frequency interval from high to low frequencies

although some run from low to high frequencies. The

source is possibly the sun (solar bursts of type II or type

III). Those at night may be trapped in ionosphere. These

have been named "sweepers » ** Various types of sweeper

activity are shown graphically, covering most of the frequency spectrum from 2 to 30 Mc/s and possibly at lower

or higher frequency. These types are normal or decreasing frequency, reverse (increasing frequency); fast (change

> 500 kc/s 2

), slow ( <25 kc/s 2) and irregular. Those

observed on mornings of Nov. 11-14, 1958 and March 13,

1959 are shown graphically. Peak occurrence is at 24.

Mc/s and majority from 23-235 Mc/s. Many sweepers

occur in trains with intervals between 4 to 140 sec. A

diurnal variation was found in rate of occurrence and distribution of sweepers by frequency. At the lowest frequencies sweepers may be identified with whistlers. (Met.

Abst. 11. 12-332. )-M.R.

89
D-246 Ghose, A. K. ; Roy, K. M. ; Gupta, S. K. et al. , On radio

measurements at Jabalpur during the solar eclipse of June 30,

1954. Institution of Telecommunication Engineers, New Delhi,

Journal, l(l):20-26, March 1955. 5 figs. , 4 refs. DBSObservations were made from June 27-July 1, 1954 (5 days ) at

Jabalpur, India, on: 1) field strength of Moscow Radio (20 m);

2) angle of incidence of reflected wave of Moscow Radio; and

3) intensity of atmospheric noise at 0.6 mc/s from direction of

belt of totality. Observations on other than eclipse dates are used as control. Path to Moscow was 5000 km. Shadow belt

lay between 2 points. Records show increase in field strength

(rapid at time of eclipse, reaching 2nd point of reflection)

then sudden drop, then sudden rise accompanied by severe

fading. Unstable F2 conditions are due to rapid succession

of events at time of eclipse. Double hop transmission changed

to single hop and vice versa between 1827 and 1927 of I. S. T.

Noise level was higher than normal and angle of reflected ray

varied more on eclipse day than normal. (Met. Abst. 7. 7-

250.)--M.R.

D-247 Gibson, John E. , Lunar thermal radiation at 35 KMC. Institute

of Radio Engineers, N. Y. , Proceedings, 46(1): 280-286, Jan.

1958. 9 figs. , 12 refs. , eqs. DLC --Measurements of the

thermal radiation of the moon were made at a frequency near

35 kmc to investigate further the variation of the radio wavelength brightness temperature with lunar phase first observed

by Piddington and Minnett at 24 Kmc. Comparison of the re- sults with calculations by Jaeger suggests the lunar surface is

composed of a layer of fine dust of very low thermal conductivity, the average depth of which is estimated as one inch or more. (Met. Abst. unpub. )--Author's abstract.

D-248 Ginzburg, V.L., O vliianii mezhduelektronnykh soudarenii

na poqloshchenie radiovoln v F-sloe i v solnechnoi korone.

(The influence of collision among electrons on absorption of

radiowaves in F layer and in the solai corona. ) Zhurnal

Tekhnicheskoi Fiziki, Moscow, 21(8): 943-947, Aug. 1951.

10 refs. , 9 eqs. DLC--Using the previous results obtained by

himself and other authors, the author derives a formula for the

calculation of the frequency of the impacts between electrons

and molecules. The use of this formula, however, requires

the knowledge of the temperature of the ionized layer, or other

corresponding data, which must be obtained independently of

the measurement of the absorption of the radio waves. In

principle, as the author shows, the measurements of this absorption might be sufficient to determine the frequency of electron-electron impacts, but this could hardly be applied in actual practice, because the electron-electron impacts would

have but very little influence upon the absorption in comparison with the electron-molecule impacts, unless the wavelength is very much larger than 200 m, and this does not seem

90
to be of practical interest. The author suggests, however,

that means for the measurements necessary for the calculation

of the frequency of electron -molecule impacts in the ionized

layers could be devised. (Met. Abst. 6D-65. )- -Physics

Abstracts, No. 338, 1953.

D-249 Giordmaine, J. A. and Alsop, L. E. (both, Dept. Physics,

Columbia Univ. ); Mayer, C.H. (U. S. Naval Res. Lab.,

Wash., D. C.) and Townes, C.H. (Dept. Physics, Col. Univ.),

A maser amplifier for radio astronomy at X-band. Institute of

Radio Engineers, N. Y. , Proceedings, 47(6): 1062-1069, June

1959. 8 figs. , 3 tables, 19 refs. , 23 eqs. DWB-The design

and operating characteristics of a maser radiometer for use in

radio astronomy at 3 cm wavelength are discussed. The operating system which is described, has a band width of 5. 5 Mc

and an input noise temperature, including background radiation into the antenna, of about 85 K. An rms fluctuation level

of about 0. 04 K is attained using an averaging time of 5 sec. A discussion of the factors determining the sensitivity of such

devices is presented. (Met. Abst. 11. 9-106. )--Authors* abstract.

D-250 Gledhill, J. A. , The behavior of the ionosphere over Cape

Town and Johannesburg during the annular solar eclipse of

Dec. 25, 1954. Journal of Atmospheric and Terrestrial

Physics, N.Y. , 16(3/4): 367-375, Nov. 1959. 7 figs.

,

table, 11 refs. DWB, DLC--Data are presented showing

the variation of the critical frequencies for the ordinary

ray in the E, Fl, and F2 regions at Cape Town and Johannesburg during the eclipse of Dec. 25, 1954. The maximum obscuration was 79% at Cape Town and 68% at Johannesburg. It was not possible to deduce a solar model

which would account satisfactorily for the data from both

stations and those from Grahamstown, published earlier.

Reasons are given for believing that oblique reflections

affected the records and it is pointed out that the plot of

foE vs. foFl, used by MINNIS to justify neglect of the re- flections, is in fact not linear throughout an eclipse.

There is some evidence for a high value of the recombination coefficient, 4 X 10-8 cnrVsec, in the E layer. (Met.

Abst. HD-41.)-Author's abstract.

91
D-251 Gledhill, J. A. (Dept. of Physics, Rhodes Univ. , Grahamstown, So. Africa), The effects of a solar eclipse on

a stratified ionosphere. Journal of Atmospheric and Terrestrial Physics, N. Y. , 18(3/4) :350-36S, Nov. 1959.

3 figs., table, 7 refs. DWB, DLC-The effects of an

eclipse on a simple three layer ionosphere, in which the

recombination coefficient decreases with height, have

been computed. The results are displayed in the form of a contour map and show relatively large tilts of the isoelectronic surfaces near the layer maxima. The development of a "valley** between the Fl and F2 layers after the

maximum of the eclipse is of particular interest. It is

pointed out that such a valley may cause considerable

errors in the interpretation of the behavior of the F2 layer.

(Met. Abst. 11D-40. )--Author*s abstract.

D-252 Golay, M.J. E. (The Perkin-Elmer Corp. , Norwalk, Conn.),

Note on the probable character of intelligent radio signals

from other planetary systems . Institute of Radio Engineers,

N. Y. , Proceedings, 49(5):959, May 1961. ref. , eq. DLC

--Detection of radio signals intelligently transmitted from

other planets and aimed at the earth is now subject to ser- ious experimental investigations. Since the use of the

1421 Mc line of hydrogen appears feasible for interplanetary radio communication, a method is outlined by which

the hypothetical space signals can be checked whether or not they are coherent. (Met. Abst. unpub. )--W. N.

D-253 Gold, Thomas (Harvard College Obs. ), Energetic particle

fluxes in the solar system and near the earth. Astrophysical Journal, Suppl. Ser. , Chicago, 4(44):408-416, June

1960. 5 figs. , 9 refs. DLC --Two modes of propagation of

high energy particles can move quickly along all the orbits

that are accessible to them in the existing field. Another

and much slower mode of propagation; in which the cosmic

ray particles gain access to new regions of space only at

the speed at which magnetic fields are convected around

by the motion of ordinary gas masses. A figure illustrates

suggested shapes of magnetic field lines resulting from a chromospheric outburst. Curves show the large decrease

of signal strength in high latitude ionospheric scatter and

cosmic noise receiver during the event of Feb. 23, 1958.

A set of curves shows ionospheric scatter records, showing the occurrence of a flare of importance 3+ and a sudden commencement of a magnetic storm nearly coincident

with a Forbush decrease, as well as the enhanced ionospheric absorption. The Van Allen flux as recorded in

Pioneer III with a Geiger counter is shown. (Met. Abst.

11. 12-230. )-E.Z.S.

92
D-254 Goldstein, Samuel J. , Jr. (Harvard College Obs. ), The

angular size of short lived solar radio disturbances.

Astrophysical Journal, Chicago, 130(2) :393-399, Sept.

1959. 4 figs., 2 tables, 7 refs. , 3 eqs. DWB, DLC--

A wide band two-element adding interferometer which ac- cepts simultaneously the radiation in the range 105-140

Mc/s was used to observe short lived solar disturbances.

The angular size of type I bursts was found to be less

than 1.6 min of arc. The average angular size of type III bursts in three clusters was 3. 2 min, and for four other

clusters an average lower limit of 3. 3 min was obtained.

The theory of these measurements is explained. (Met.

Abst. 11. 9-111. )--Author's abstract.

D-255 Gonze, R. and Pourbaix, E. , Altitudes de radiation . (Radiation heights. ) Ciel et Terre, Brussels, 76(11/12):

394-402, Nov. /Dec. 19S0. 6 figs. , 9 refs. DWB, DLC--

Statement of a new method, still in progress, which permits to establish the radiation heights in the solar atmosphere for the various radio frequencies, according to geomagnetic observations made at Manhay and to observations

on 800 and 15C MHz made at Humain and on 27 KHz at

Uccle. All the results are in fair agreement and it seems

admissible that, in the instance of quiet or little disturbed

solar conditions, the difference of radiation height in connection with electron density is relatively constant. Certain radioelectric recordings enabled the determination of

apparent variation of the radiation height difference during

the development of an important solar flare. Finally, the

close parallelism is pointed out between the apparent var- iation of the radiation height difference and the development of radioelectric surges, as well during the time when

these latter are increasing as when they are decreasing.

(Met. Abst. unpub. )--A. V.

D-256 Goodman, J. and Lebenbaum, M. , A dynamic spectrum

analyzer for solar studies. Institute of Radio Engineers,

N. Y. , Proceedings, 46(1):132-135, Jan. 1958. 4 figs.,

8 refs. DLC--A spectrum analyzer of the type originally

built by Wild and Sheridan is described. The analyzer

covers the range of 90 Mc to 580 Mc at a rate of 3 sweeps

per second in three overlapping bands. The output information is presented on three high resolution oscilloscopes

in a frequency intensity display, and the time axis is provided by the continuous motion of the film used to photograph the displays. Modifications and improvements are suggested. (Met. Abst. unpub. ) --Authors' abstract.

93
D-257 Gopal Rao, M.S.V. and Rao, B. Ramachandra (both,

Andhra Univ. , Waltair), Effect of solar eclipse of June 20

1955 on long distance shortwave transmissions . Current

Science, Bangalore, 24(12):408, Dec. 1955. fig., 3 refs.

DLC --Signal strength data as obtained between 0700 and

1000 hr and during night on 9. 52 Mc/sec at Waltair (lat.

17 41') by a Hallicrafters type 5x-42 receiver show some

peculiarities when the records before, during and after

the eclipse were compared. Insignificant influence of the

D region absorption on signal strength is shown and sudden fading during eclipse is discussed briefly. (Met.

Abst. 8. 1-353.) --W.N.

D-258 Gopal Rao, M.S.V. ; Rao, B. Ramachandra and Ramachandra Rao Pant,P. (ail, Andhra Univ. , Waltair, S.

India), Fading of C. W. signals as a means of spread F

study. Current Science, Bangalore, 29(8):304-305, Aug.

1960. fig., table, 6 refs. DWB, DLC -In recent years

considerable evidence has been accumulated to show that

ionospheric irregularities are the cause of radio star scintillations. The irregularities can be used to study spread

F irregularities. An experiment is described when C. W.

signals from Colombo radio station in Ceylon were recorded by Hollicrafters receiver type in combination with a conventional D.C. amplifier. During the months of Jan.

and Feb. 1959, 100 C. W. records were taken. All these

records show an increase in fading rate whenever spread

F is observed. (Met. Abst. unpub. )--A. H. K.

D-259 Gordon, W. E. , Incoherent scattering of radio waves by

free electrons with applications to space exploration by

radar. Institute of Radio Engineers, N. Y. , Proceedings,

46(11): 1824-1829, Nov. 1958. fig., 6 refs. , 13 eqs.

DWB--Free electrons in an ionized medium scatter radio

waves weakly. Under certain conditions only incoherent

scattering exists. A powerful radar can detect the incoherent backscatter from the free electrons in and above the

earth's ionosphere. The received signal is spread in frequency by the Doppler shifts associated with the thermal

motion of the electrons. On the basis of incoherent backscatter by free electrons, a powerful radar, but one whose

components are presently within the state of the art, is

capable of: 1) measuring electron density and electron

temperatures as a function of height and time at all levels

in the earth's ionosphere and to heights of one or more

earth's radii; 2) measuring auroral ionization; 3) detecting transient streams of charged particles coming from

outer space; and 4) exploring the existence of a ring current. The instrument is capable of 1) obtaining radar echoes from the sun, Venus, and Mars and possibly from

94
Jupiter and Mercury; and 2) receiving from certain parts

of remote space hitherto undetected sources of radiation

at meter wavelengths. (Met. Abst. 11. 2- 169. )- -Author's

abstract.

D-260 Graham Smith, F. (Mullard Radio Astronomy Obs. , Cambridge), The spectrum of galactic radio emission. Nature,

London, 191(4796): 1381, Sept. 30, 1961. 4 refs. DWB,

DLC--TUNMER and HOYLE have accounted for the general

radio emission from the Galaxy as the synchroton radiation

of high energy electrons in a magnetic field. In this note

it is shown that the expected energy spectrum of the cosmic ray electrons is not consistent with the observed radio

spectral index. (Met. Abst. unpub. )--R. B.

D-261 Grant, Lewis J. , Jr. , A suggested design project on an

orbit rocket . Journal of Space Flight, 3(1): 1-5, Jan. 1951.

2 refs. DLC--A suggestion and an outline for planning an

"orbiter" for the purpose of obtaining necessary information

and data to make possible the establishment of a space

ship. Meteorological data that may be obtained by instruments aboard the "orbiter" are: variability of the solar constant, air density, albedo of earth, and cloud pattern over

a long period of time (from 500 miles up); auroras, power,

size and ionization potentials of cosmic rays, long period

recording of meteor hits (and the orbiter itself), temperature drop in the earth's shadow, and conditions of radio

reception on the "orbiter." (Met. Abst. 4. 4-48. )--W. N.

D-262 Graves, Carl D. (Space Technology Labs. , Inc., L.A. , Calif.), Radio propagation measurements using the Explorer VI satellite. (Summary only). Journal of Geophysical Research, Wash., D. C, 65(9): 2585-2587, Sept. 1960.

4 refs. , 6 eqs. DLC--This paper presents the results of an

experiment to measure the electron density above the ionosphere. The experiment utilized two coherent signals, one

VHF and one UHF, transmitted from the Explorer VI satellite. The evidence of our data is that the electron concentration in the vicinity of the satellite, 18, 000 km above the

earth, was unusually high, of the order of 10^ electrons/

cm3. However, the results were influenced by unexpectedly high correction factors and possibly by an intense

world-wide magnetic storm that occurred during the measurement period. (Met. Abst. 11. 12-370. )--Author's abstract.

95
D-263 Gringauz, K.I. ; Kurt, V. G. ; Moroz, V.I. et al. (all,

Radio Eng. Inst. Acad. Scien. , USSR), Resul'taty nabliudenii poluchennye pri pomoshchi lovusbek zariazhennykh

chastits na sovetskikh kosmicheskikh raketakh do R - 100, 000 km. (Results of observations of charged particles

observed out to R- 100, 000 km, with the aid of charged

particle traps on Soviet space rockets. ) Astronomicheskii

Zhurnal, Moscow, 37(4): 716- 735, July/Aug. 1960. 11 figs.,

3 tables, 26 refs. , 11 eqs. English summary p. 713. DLC.

Transl. in Soviet Astronomy AJ, New York, 4(4):680-395,

Jan. /Feb. 1961. DLC --Results of the reduction measurements made with the aid of trielectrode ion traps mounted

in the Soviet space ships launched on Jan. 2 and Sept. 12,

1959, are presented. Rocket trajectories out to R < 100, 000

km were studied. The potential of the container, which was

immersed in a hydrogen plasma and subject to the action of

electrons present in the radiation belts and to short wavelength radiation of solar origin, is discussed. Values for

the container potential, computed with different values as- signed to temperature, plasma concentration, and density

of photo-current at the container surface, are tabulated. The

plasma density was estimated with the ion trap outer grid

at zero potential. The motion of the container and the effect of radiation belt electrons on collector currents were

calculated. Since all of the ion traps were insensitive to

the radiation belt environment (as shown by the absence of

sizeable negative currents in all of the traps), it is concluded that the flux of radiation belt electrons over the re- gion R < 50, 000 km does not exceed 3. 10* cm"^ sec"-'- for

electrons of energy E > 200 ev. In the region 50, 000 km

< R <. 75, 000 km, negative currents were recorded in

all the traps, corresponding to an electron flux at energy

E > 200 ev of about 2. 10° cm"2 sec"-*-, which supports the

existence of a new, ulterior radiation belt. An ion density

of the order of several hundred ions/cm^ was found out to

15, 000 km. The density falls off farther out, and only an

estimate can be offered for the upper limit of density at

R < 20, 000 - 22, 000 km, nt < 30 - 80 cm'3. This supports the view that polarization of the zodiacal light is entirely due to the dust component, while the high electron

density found from studies of atmospheric whistlers relates

to the geocorona. (Met. Abst. unpub. )- -Authors' abstract.

D-264 Gringauz, K.I. and Rudakov, V.A. , Izmerenie olektronnoY konsentratsii v ionosfere po vrashcheniiu plokosti

poliarizatsil radiovoln, izluchaemykh s raket . (Determination of electron concentration in the ionosphere from

rotation of the plane of polarization of radio waves emitted

by rocket.) Akademiia Nauk SSSR, Doklady, 132(6):1311-

1313, 1960. 2 figs., 2 refs. , 2 eqs. DLC--

96
Two formulas for calculation of the distribution of radiowaves in the ionosphere considering the magnetic field of

the earth. The rocket (unmanned) launched Aug. 27, 1958,

reached 450 km. Calculation methods based on consideration of Faraday effects. Part of a graph showing the level

of signals at various frequencies. Profile shows correlation between calculated and obtained data. (Met. Abst.

unpub. )--E. Z. S.

D-265 Gringauz, K.I. , Raketnye izmerenifa elektronnoi kontsentratsii v ionosfere pri pomoshchi urtrakorotkovolnovogo

dispersionnogo interferometra. (Rocket measurements of

the electron density in the ionosphere using ultrashort

wave dispersion interferometers.) Iskusstvennye Sputniki

Zemli, Moscow, No. 1:62-66, 1958. 4 figs. , 8 refs. , 4

eqs. DLC--The author presents the results of measurements of the vertical distribution of electron concentration in the ionosphere from high altitude geophysical rockets released in the U.S.S. R. during 1954-1955 — one

rocket attained a height of 473 km. The determination of

electron concentration involved the use of a dispersion

interferometer to measure the dispersion of radio waves

emitted by a rocket. The rocket, which was released at a small angle to the vertical, was equipped with a transmitter emitting radio waves in the ultraviolet range with a frequency of f , and f „ = P f . . The radio waves from the

rocket were received at two points on the earth and the

phase differences and level of oscillations received were

recorded continuously. The coordinates of the rocket were

measured simultaneously by optical radio methods and the

ionosphere was probed by means of a panoramic ionosphere

station close to the point of rocket release. The results of

measurements, which are presented, concern frequencies of

f 1 = 48 X 10S H z and f 2

= 144 X 106 H Z (P = 3). The

coefficient of refraction N, was computed by the equation

N, ~ 1 -

m 2 Ne

1 2TTmt Z

(N - effective concentration of electrons, e and n - charge

and mass of electron, - frequency in Hz

. ) The phase difference of the two receivers referred to the higher frequency is given by

97
NtneM

The variation of (T) with variation of L from L to L + AL,

taking into account^ , is given by

ACZU

r 7rL€

e %fJ

and the mean value of N over £^. L is given by

The rockets were released in middle latitudes. The re- sults of the measurements relative to the region lying below the maximum F ionization indicate that a clearly marked E layer does not exist. The active height, at which

radio waves of the ionospheric station in the F layer are

reflected, lies 50-150 km lower than the active heights

recorded by the ionospheric station. (Met. Abst. HE- 55. ) --I.L.D.

D-265 Gruber, S. (M.I.T. , Camb. , Mass.), Statistical analysis of radio star scintillation. Journal of Atmospheric and

Terrestrial Physics, London, 20(1):59-71, Feb. 1961. 7

figs. , 7 refs. , 9 eqs. DLC --Radio star scintillation data

are analyzed by statistical techniques to find the autocorrelation functions and power density spectra of the fluctuations in amplitude and phase. Interpretation is given

in terms of a drifting phase changing screen as postulated

by BOOKER, RATCLIFFE and SHINN. It is shown how the

drift velocity of the irregularities in ionospheric electron

density that lead to the scintillations, as well as the

mean square amplitude and phase of the fluctuations, may

be obtained from these records. --Author's abstract.

D-267 Guier, William H. and Weiffenbach, George C. (both.

Applied Physics Lab. , Johns Hopkins Univ. , Silver Spring,

Md. ), Theoretical analysis of Doppler radio signals from

earth satellites. Nature, London, 181(4622): 1525- 1526,

May 31, 1958. 2 tables, 2 eqs. DWB--A brief description is given of the method of determining the orbit of an

artificial satellite from measurements of the Doppler shift

of its radio signals. A detailed description of the present

analysis will be published in the future. (Met. Abst.

12. 2-45. )»N. N.

98
D-268 Gustafsson, Georg; Egeland, Alv and Aarons, Jules,

Audio frequency electromagnetic radiation in the auroral

zone . Journal of Geophysical Research, Wash., D. C.

,

65(9):2749-2758, Sept. 1960. 9 figs. , table, 18 refs.

DLC --During three one-month periods, continuous spectrograms of the electromagnetic energy in the spectral region

between 10 cps and 10 kc/sec were recorded in Kiruna,

Sweden. The records were examined from the viewpoint of

background energy. Throughout the entire frequency band

studied, there is a low daytime signal level and a nighttime maximum. The ratio of the maximum to minimum amplitude varies as a function of frequency (the higher maximum-to-minimum ratio occurs at the lower frequency range

of 20 to 200 cps) and with the season of the year. It is

concluded that the daytime ionosphere absorbs the energy

throughout the entire spectrum studied. It was found that,

although strong deviations of the signal level from the

normal were often associated with geomagnetic disturbances, there was a general lack of correlation between

magnetic index and low frequency noise, except in the

10- to 45-cps frequency range. The origin of the background signals is probably two-fold, atmospherics from

great distances, as well as magnetic and exospheric fluctuations contributing to the lower band. On eleven oc- casions, electromagnetic radiation associated with micropulsations of the earth's magnetic field was detected.

Two frequency bands were identified; one centered at

750 cps, which is the gyro frequency for protons at an

altitude of 100 km above Kiruna; and the other ranging

between 1. 8 and 4. 5 kc/s, which has been identified as

hiss. On all but one of the occasions when emissions

were detected, the 750 cps signals were quite stable in

frequency. During four of the longest periods when radiation was recorded, the low frequency emissions were re- ceived between two phases of a magnetic storm; micropulsations were simultaneously evident on the Kiruna

magnetograms. (Met. Abst. 11. 12-324. ) --Authors' abstract.

D-269 Hachenberg, Otto, Sonnentatigkeit und Ausbreitung der

elektrischen Wellen in der Erdatmosphlre. (Solar activity

and propagation of electrical waves in the earth's atmosphere. ) Leipzig, Urania-Verlag, 1S55. 27 p. 10 figs.

Gesellschaft zur Verbreitung Wissenschaftlicher Kenntnisse. Vortragsreihe Naturwissenschaften, Vol. 13.

DLC--A pamphlet giving the basic material, with illustrations, of a popular science lecture on the ionospheric

structure, ionospheric propagation of radio waves and

sounding by impulses or waves, and solar ionizing influences on the ionosphere. The separate layers (D, E, Fl

99
and F2) and their formation are treated in detail, and re- cords are reproduced showing variations and characteristics of these layers, or disturbances in the layers.

(Met. Abst. 7. ll-6.)-M.R.

D-270 Hachenberg, O. and Kruger, A. (both, Heinrich-HertzInst. , der Deutschen Akad. Wissenschaften zu Berlin),

The correlation of bursts of solar radio emission in the

centimetre range with flares and sudden ionospheric disturbances. Journal of Atmospheric and Terrestrial Physics,

N. Y. , 17(1/2): 20-33, Dec. 1959. 9 figs. , 2 tables, 16

refs. DWB, DLC--From statistical investigations of solar

flares, of bursts of solar radiation in the centimetre range

and of the accompanying effects of sudden ionospheric

disturbances (SID) recorded during the first S months of

the IGY, it follows that there exists a close correlation

between bursts in the centimetre range and SID. Only

those flares, which give rise to a centimetre burst, are also able to cause a SID. Both flares and the ionizing

radiation of the ionospheric D layer have their origin in

the chromosphere. The close correlation confirms our view that the ionizing radiation, as well as the centimetre

radiation of the flares, are generated by super thermal electrons. The ionizing radiation is evidently a "Bremsstrahlung" of the X-ray region. (Met. Abst. 11D-44. ) --Authors'

abstract.

D-271 Hachenberg, O. and Volland, H. , Vergleich zwischen

3. 2 cm Radiostrahlung der Sonne und ionosphifrischer

Dampfung im D-Gebiet wahrend einer Sonneneruption.

(Comparison between 3. 2 cm radio emission from the Sun

and ionospheric damping in the D layer during a solar

eruption. ) Zeitschrift fur Astrophysik, Berlin, 47(2):69-

80, 1959. 4 figs., table, 12 refs. , 24 eqs. DLC--The

time variation of the nondeviative absorption in the ionospheric D layer during a sudden ionospheric disturbance

(Mogel-Dellinger effect) is compared with the radio burst

on 3. 2 wavelength caused by the corresponding solar

flare. Using the continuity equation for the ionospheric

electron density, the intensity variation of the ionizing

radiation can be determined. It is found that this intensity variation is in qualitative agreement with the intensity variation of the 3. 2 cm emission. Thus the hypothesis is strongly supported, that the 3. 2 cm emission and

the ionizing radiation responsible for the D layer both

originate from the same gaseous volume in the solar atmosphere, and are both generated by similar emission

mechanisms. (Met. Abst. 11. 12-53. )--Authors' abstract.

100
D-272 Haddock, F.T. , Introduction to radio astronomy. Institute of Radio Engineers, N. Y. , Proceedings, 46(1):3-12,

Jan. 1958. 3 figs. , 108 refs. DLC--A general description of the nature of radio astronomy, its differences from

optical astronomy, a review of the earliest beginnings of

galactic and solar astronomy, and a listing of other important observational discoveries are given. A nearly

complete bibliography (108 entries) of these early publications and of the principal review books and papers on

radio astronomy is given. Some practical aspects and

instrumental developments of possible interest to radio

engineers are pointed out. The papers (50) in the present

issue of the Proceedings of the IRE are discussed generally and individually. A brief discussion of some new

results on solar burst spectra obtained at the Radio

Astronomy Observatory at the University of Michigan,

is presented. Jansky's 14. 5 m rotatable directional an- tenna and his 31 ft reflector are illustrated. (Met. Abst.

unpub. )--Author's abstract.

D-273 Haddock, F.T. (Mich. Univ., Ann Arbor), Report on

URSI Commission V; Radio astronomy. National Research Council, Wash., D. C, Publication, No. 581:

115-118, 1958. Also issued as Institute of Radio Engineers, Proceedings, 46(7): 1373 -1375, July 1S58. DWB,

DLC--The Commission on Radio Astronomy is concerned

with international exchange of scientific data, theory,

programs of investigations and coordination of observational programs on an international scale, continuous

monitoring of solar radio emissions, radio emission, co- ordination of ursigrams, etc. Radio astronomers from

over a dozen nations attended the conference. A summary is given of the work done recently in study of solar

radio research, radio sources, radio propagation, radio

waves in the Galaxy and radio planetary system emissions

from the planets. (Met. Abst. 11. 8-145. )-M. R.

D-274 Hagen, John P. and Hepburn, Nannielou, Solar outbursts

at 8. 5 mm wavelength. Nature, London, 170(43x9): 244-

245, Aug. 9, 1952. fig. , table, 9 refs. DWB-During

May through Sept. 1951, 5 bursts of solar radiation on

8. 5 m were recorded at Washington, 4 accompanying

flares and sudden ionic disturbances. Records are shown.

(Met. Abst. 4.9-104.)

D-275 Hagen, J. P. (Naval Res. Lab. , Wash. ,D.C), The ex- ploration of outer space with an earth satellite. Institute

of Radio Engineers, N. Y. , Proceedings, 44(6): 744-747,

June 1956. 5 figs. DLC--

101
Sometime during the coming Geophysical Year (July, 1957

to Dec. 1958) an attempt will be made to launch an artificial satellite in an orbit around the earth. The Office of

Naval Research has been assigned the responsibility to

perform this task and has established Project Vanguard in

the Naval Research Laboratory to carry it out. The Dept.

of Defense turned to the Navy to manage this triservice

project because of its extensive experience in upper atmosphere research with rockets. The satellite which Project

Vanguard intends to launch in an orbit is a small one, yet

must be a research vehicle. The National Committee for

the IGY of the National Academy of Sciences has established a panel which is concerned with the nature of the

scientific experiments to be done in the vehicle. Work is

in progress, not only on the vehicles, but on the experiments to be done in the satellite. Experiments conducted

in an artificial earth satellite circling the earth in the

outer tenuous region of our atmosphere can greatly increase our knowledge of the atmosphere --its structure,

its constituents, and the powerful radiations, both electromagnetic and corpuscular, that impinge upon it and

help determine its state. (Met. Abst. 8. 1-133. )--Author's

abstract.

D-276 Hagen, J. P. (Naval Research Lab. ), Radio tracking,

orbit and communication for the earth satellite. Aeronautical Engineering Review, N. Y. , 16(5):62-66, March 1957.

3 figs. DLC--A chain of receiving stations, extending

from Washington, D. C. to Santiago, Chile, is being set

up to create a radio fence which will intercept a satellite

each time it circles the earth. This system was chosen

to prove that a satellite is in orbit and to derive geophysical information from perturbations of that orbit. (Met.

Abst. 9. 7-71.)--Author's abstract.

D-277 Hakura, Y. and Goh, T. , Pre-SC polar cap ionospheric

blackout and type IV solar radio outburst. Japan. Radio

Research Laboratories, Journal, 6:635-850, Oct. 1959.

--Short wave radio blackouts in polar cap regions are often

found to occur well before the sudden commencement of

magnetic storms and this phenomenon is closely corre- lated with the occurrence of type IV solar RF bursts. A

possible explanation of these effects is given which is

consistent with other related phenomena such as cosmic

ray storms. IRE Abst. 1223

102
D-278 Hamburg. Meteorologisches Observatorium, IonospharenBericht. (Ionospheric report. ) First issue received, v. 5, no. 1, Jan. 1/10, 1953. Latest issue seen, v. 6, no. 37,

Dec. 27/31, 1954. 4 p. per issue, graphs. Issued with

collaboration of the Arbeitsgemeinschaft Ionosphare, at

Darmstadt. DWB--Routine features: current data and re- view of earth magnetic and ionospheric disturbances, relative sunspot numbers, schematic sunspot charts, limiting

frequency of the F2 layer, geomagnetic amplitudes, solar

eruptions, bursts, corona observations, maximum frequency of the sporadic E layer, geomagnetic characteristics,

ultraradiation and radiation of longest waves. (Met. Abst.

SD-173.)--A.A.

D-279 Hame, T. G. and Kennaugh, E. M. (both, Ohio State Univ.),

Recordings of transmissions from the Satellite 1958 A 2

at the Antenna Laboratory, Ohio State University. Institute

of Radio Engineers, N. Y. , Proceedings, 47(5, Pt. 1):991-

992, May 1959. fig., table, 2 refs. DWB--Observations

of the radio transmissions from the Russian Satellite 1958

2\ 2 (Sputnik III) were carried out at the Antenna Laboratory Field Station, Ohio State University, Columbus. The

signal characteristics of transmissions from Sputnik I on

20. 005 mc and that of Sputnik III are compared. During

Nov. 1958 to Jan. 1959, the period varied between 39 and

52 seconds. It was observed that a severe amplitude fading, not due to Faraday rotation, had become superimposed

on the transmission from Sputnik III. This is illustrated

in two orthogonal polarization graphs. (Met. Abst. 11E59. )-N. N.

D-280 Harang, L. and Pedersen, K. , Drift measurement of the

E layer during the solar eclipse June 30. 1954. Journal of

Atmospheric and Terrestrial Physics, 10(l):44-45, Jan.

1957. 2 figs. , ref. DWB- -Records on 2 Mc/s of E layer

drift at Kjeller, Norway, on June 30 are compared with

those on July 1 and 2. On eclipse day a normal E layer

was embedded in an Es layer at a somewhat greater height.

During eclipse drift changed from NE-SW and back again.

(Met. Abst. 8. 6-182. )-C.E. P. B.

D-281 Harang, L. and Troim, J. (both, Norwegian Defence Res.

Estab. , Kjeller, Norway), An example of heavy absorption in the VHF band in the Arctic ionosphere. Planetary

and Space Science, N. Y. , 1(2):102-104, April 1959. 3

figs. , ref. DWB--From records of meteor echoes on 40

Mc/s and of scintillations from the Cassiopeia source on

45 Mc/s, it is shown that on July 7, 1958, in the early

morning hours, a very heavy absorption appeared. The

meteor echoes disappeared completely and the radiation

103
from Cassiopeia diminished to less than 1/5 of its normal

value. The observations were made at Tromso k6 = 70 N)

and in the direction toward the auroral zone. A great geomagnetic storm appeared with a sudden commencement at

08. 40 MET, the geomagnetic storm started about 5 hr after

the absorption effect of the ionosphere had started. (Met.

Abst. 11. 12-439. )- -Authors' abstract.

D-282 Harris, I.; Jastrow, R. and Cahill, W. F. (all, Theoretical Div. , Nat'l. Aero, and Space Admin. , Wash. , D. C. ),

Determination of satellite orbits from radio tracking data.

Institute of Radio Engineers, N. Y. , Proceedings, 47(5,

Pt. l):851-854, May 1959. fig. , 2 tables, 9 eqs. DWBA computer program has been developed which permits an

approximate determination of a satellite orbit for a minimal

amount of tracking data. (Met. Abst. 11. 6-151. ) --Authors'

abstract.

D-283 Harrison, V.A. W. (Radio Res. Station, Slough), Ionospheric effects associated with the solar flare of July 10,

1959. Nature, London, 186(4720) :228-229, April 16, 1960.

3 figs. , 3 refs. DWB--On July 10, 1959, Sydney Observatory reported a class 3+ solar flare lasting from 0210 to

0410 U.T. The Cable and Wireless, Ltd. , receiving station at Singapore also experienced a sudden fadeout of all

radio circuits at 0210 U.T. , the circuits not being reestablished until between 0415 and 0430 U.T. Ionospheric

changes associated with the flare were observed at Singapore by using an automatic ionosonde. Calculations and

deductions suggest that the enhanced ionization of the F2

layer on July 10 can reasonably be attributed to the effects

of the solar flare. (Met. Abst. 11. 12-429. )--E. Z. S.

D-284 Hartz, T. R. , Radio star scintillations and the ionosphere.

Canadian Journal of Physics, Ottawa, 33(8):476-482, Aug.

1955. 5 figs., 6 refs. DWB, DLC-The observed intensity

at the surface of the earth of radiation at a frequency of

50 Mc/s from a radio star has been studied. A relationship is shown to exist between the fluctuations, or scintillations, in this observed radiation intensity and the an- gle of its incidence on the 400 km level of the earth's ionosphere. The occ/irrence of these scintillations is compared with other ionospheric phenomena as determined by

vertical soundings from the earth. The probable cause of

the fluctuations has been localized to a source in the high

ionospheric regions. (Met. Abst. 11E-60. )--Author's

abstract.

104
D-285 Hartz, T. R. , A solar noise outburst of Jan. 15. 1955.

Nature, London, 175(4464): 908-909, May 21, 1955. DWB

--A large noise outburst from the sun was recorded on 50

Mc/s at Ottawa on Jan. 15, 1955. It was followed by an

intense ionospheric storm and an intense auroral display

on Jan. 17-18. (Met. Abst. 6. 8-20. )--C. E. P. B.

D-286 Hartz, T. R. , Solar-terrestrial relations . Canada. Defence Research Telecommunications Establishment, RPL

Report No. 23-2-3, Feb. 1958. 61 p. 40 figs., 2 tables,

75 refs. At head of t-p: Defence Research Board. DWB

(M(055) C212rpL)--The interrelation of phenomena on the

sun and in the earth's ionosphere has been studied in

order to establish a causal dependence which could result

from travelling solar particles. In addition to the examination of a variety of data from a number of sources, an ex- tensive r-f noise recording program was undertaken to provide information on those regions of the solar and terrestrial atmospheres from which optical data were not available. The occasion on which there was an influx of solar

particles into the earth's ionosphere were established from

magnetic data, from optical observations of the Polar Aurora, and from h-f and v-h-f radio observations close to the

auroral zone. On the basis of these data the ionospheric

disturbances for a 12 month period were related to prior

distinctive solar events that were considered capable of

producing the high energy particles. The selection was

made from the optical, spectroscopic and radio data available. It was found that solar flares, eruptive prominences, and disappearing filaments were the most frequent

sources of Earth reaching particles, and that large sunspots contributed only occasionally to ionospheric disturbances. Moreover, the radio noise data permitted a fairly

reliable estimate of the particle velocities in the solar

corona, which could be used to predict the probability of

subsequent terrestrial effects of the ejected particles. A

correlation coefficient of 0. 65 was found between probabilities predicted from the solar information and observed

ionospheric disturbances which occurred two or three days

later. The observational evidence on the solar noise

bursts and on ionospheric storms could be explained only

on the basis of a considerable distribution of velocities

for the particles ejected from the sun. It was shov/n that a Maxwellian distribution of corpuscular velocities was a probable one. Moreover, the observations indicated that

particles are frequently emitted from the sun with a distribution of velocities, but that only in the case of very large

phenomena are there sufficient particles with the high

energies necessary to overcome the sun's gravitational

field and reach the earth. --Author's abstract.

105
D-287 Harvard Univ. Harvard College Observatory, The effects

of the terrestrial atmosphere on radio waves from outer

space; Report on a conference held at Harvard, May 10,

1S5S. 9 p. mimeo. Unchecked.

D-288 Haskell, R.E. and Holt, E.H. (both, Rensselaer Polytechnic Institute, Troy, N. Y. ), Representation of propagation parameters for the plasma in a magnetic field.

Institute of Radio Engineers, N. Y. , Proceedings, 49(10):

1584, Oct. 1961. 4 figs., 3 refs. , 4 eqs. DLC -The effect of a dc magnetic field is discussed and demonstrated

by extending the plane propagation field curves by Bachyinski et al to 3-D models given. (Met. Abst. unpub. )--

W.N.

D-289 Hatanaka, Takeo, Faraday effect in the earth's ionosphere with special reference to polarization measurements

of solar radio emission . Cornell Univ. School of Electrical Engineering, Contract AF 19(604) -73, Scientific Report, No. 5, Aug. 30, 1955. 18 p. 5 figs. , 8 refs. , 34

eqs. Also pub. as Astron. Society of Japan, Publication,

8(2):73-86, 1956. --The author and co-workers found that

the polarized bursts from the sun were a mixture of a ran- domly polarized and an elliptically polarized component,

with the ellipticity dependent on position of source in the

sun's disk. The axis of the ellipse is rotated somewhat

by the Faraday effect in the earth's ionosphere, but unless

total electron density along path of radio wave through ionosphere is known, the original orientation of the axis cannot be obtained. The paper deals with the calculation of

the Faraday effect in the ionosphere. The general expression is given and then applied to the simple case when the

only effect is the rotation of the axis of the ellipse. (Met.

Abst. HE-62.)-M.R.

D-290 Hatanaka, T. , Issledovaniia Solntsa v Iaponii . (Solar

studies in Japan. ) Priroda, Moscow, No. 8:77-81, Aug.

1959. 7 figs. DLC--This review of solar studies made in

recent years in Japan includes detailed information on investigations of solar activity carried out by optical methods and with the aid of radio waves. The optical observations are made at the Tokyo Astronomical Observatory of

Tokyo University, while the radioastronomical studies are performed by both the Tokyo observatory and the Institute

of study of Atmospheric Phenomena at Toyokava near

Nagoya. Numerous photos and graphs illustrating the

text are included. (Met. Abst. 11. 12-83. )--A. M. P.

106
D-291 Haviland, R.P. (Special Defense Projects Dept. , General

Electric, Philadelphia), What the future holds for the earth

satellite. General Electric Review, Schenectady, N. Y.

,

59(5):10-16, Sept. 1956. 10 figs., 2 tables. DLC--The

possible orbits and respective areas of the earth which

could be seen from a satellite at 300 mi, 4000 mi; or the

areas over which a satellite at 22, 300 mi height could re- lay radio or TV signals from hemisphere to hemisphere or within the Western Hemisphere are shown on maps. Tables

give distances of vision, field of view, etc. , for heights

of 257, 620, 1210, 2222, 4000, 7650, 19, 000 and 22, 300

mi. Weather charting and forecasting possibilities are also considered. Hurricanes, clouds, albedo and solar

radiation could be measured or observed from such a station. (Met. Abst. 9. l-94.)--M.R.

D-292 Haviland, R.P. (Missile and Space Vehicle Dept. , General Electric Co. Philadelphia, Pa.), Doppler shift effects

in space propagation. Institute of Radio Engineers, N. Y.

,

Proceedings, 49(11): 1694-1695, Nov. 1961. ref. , 11 eqs.

DLC--In a solar ionosphere, various effects of changes in

the propagation medium may become imperative, hence,

five non-steady-state cases are theoretically examined, and

their individual Doppler shifts estimated. (Met. Abst. un- pub.)-W.N.

D-293 Hayre, H.S. (Univ. of N. Mexico, Albuquerque), Radar

scattering cross section applied to Moon return. Institute

of Radio Engineers, N. Y. , Proceedings, 49(9):1433, Sept.

1961. 10 refs. , 5 eqs. DLC--This brief theoretical calculation, as applied to pulse radar and compared with the

radar equation, indicates a rough effective moon surface

rathe/ than a quasi-smooth surface as is assumed by some

other research workers. --W. N.

D-294 Herbays, E. and Coutrez, R. , Frequences reservees pour

la radioastronomie. (Reserved frequencies for the radioastronomy. ) International Scientific Radio Union, Brussels,

Bulletin d'Information, No. 121:14-19, May/June 1960. DLC

—Report of the efforts of the radioastronomers to obtain the

safeguard of the frequency bands used for radioastronomical

observations. The International Union of Telecommunications made a study of this question introduced in the form

of two resolutions expressed at the 11th General meeting of

the ISRU in 1954. Mention is made of the frequency bands

reserved for radioastronomy in the different regions into

which the globe has been divided. The end of this article

constitutes a summary of the recommendations made by the

ISRU for the safeguard of the frequencies used for radioastronomical observations. --A. V.

107
D-295 Herrinck, Paul (Chef du Bureau de Geophysique du Service

Meteorologique du Congo Beige et du Ruanda-Urundi), Analyze

de la variation annuelle et semi-annuelle de la frequence critique de la couche F2 a Leopoldville-Binza. (Analysis of the an- nual and semi-annual variation of the critical frequency of the

F2 layer at Leopoldville-Binza. ) (In: Angola. Servico Meteorologico, Miscelanea geofizica, Luanda, 1956. p. 155-162. 4 figs.

,

2 tables. ) DWB--Since only the annual and semi-annual amplitude variations are important, it is shown how good local foF2

forecasts can be made by considering each hour of the day, and

using average foF2 values derived from sunspot forecasts. --G.T.

D-296 Hewish, A. (Mullard Radio Astron. Obs. , Cavendish Lab. ), Extrapolation of the number-flux density relation of radio stars by

Scheuer's statistical method. Royal Astron. Soc. , London, Monthly Notices, 123(2): 167-181, 1961. 12 figs. , 6 refs. DLC--An attempt is made to assess the usefulness of Scheuer's statistical

method of analyzing the records derived from a phase switching

receiver. A Monte Carlo technique is described which enables

the probability distribution of recorded deflections to be computed in EDSAC for any assumed distribution of radio sources.

Some typical models are considered and it is concluded that,

subject to a small enough receiver noise, the statistical method

gives information about the source distribution at flux densities

considerably lower than those at which the sources may be

counted individually. The method is applied to observations at

178 Mc/s using the method of aperture synthesis. It is shown

that the log N-log S relation cannot have a uniform slope of -1. 5.

A slope of -1.8 yields good agreement provided the source density is suitably truncated at small flux densities. --Authors abst.

D-297 Hewish, A. , The diffraction of galactic radio waves as a method

of investigating the irregular structure of the ionosphere . Royal

Soc. of London, Proceedings, Ser. A, 214(1119):494-514, Oct. 9,

1952. 13 figs. , tables, 16 refs. , 6 eqs. DWB--Amplitudes of 1.4

-8 m waves from 4 radio stars at 2 points 1 km apart show that

variations of phase and amplitude are due to steady drift of an

irregular wave pattern, which can be regarded as caused by ionospheric irregularities 2-10 km across with a variation of electron content of about 5 X 10§ per cm , in a thin layer at a height

of about 400 km. They are most pronounced about midnight. The

irregular part of the ionosphere has a wind-like motion; the E-W

component varies from + 500 m/s to -500 m/s. The average is

about 300 m/s at 0-1 h, decreasing to 150 at 4-5 h. Large speeds

are associated with magnetic disturbances. (Met. Abst. 4. 10-110)

--C. E. P. B.

D-298 Hewish, A. (Cavendish Lab. , Cambridge), The Scintillation

of radio stars. (In: Beer, Arthur (ed. ), Vistas in Astronomy.

London, Pergamon Press, 1955. Vol. 1:599-606. 2 tables,

19 refs.) DLC (QB3. B35) -The intensity and apparent

position of radio sources are observed to fluctuate in a manner

analogous to the scintillation of visual stars.

108
Experiments are described which show that the scintillation

is caused by diffraction of the incoming waves by irregularities of electron density in the upper ionosphere. The

origin of the irregularities is not known and the solution

may raise problems of astronomical interest. A phenomenon similar to scintillation occurs when a radio source is

viewed through the solar corona, and this fact enables deductions to be made about the irregular structure of the

corona at distances in the range 5-15 solar radii. (Met.

Abst. 10. 3-201. ) --Author's abstract.

D-299 Hey, J. S. , Solar radiations in the 4-6 metre radio wavelength band. Nature, London, 157(3876) :47 -48, Jan. 12,

1946. Note by F. J. M.Stratton, Ibid., p. 48. DLC--Hey

reports on the observation of solar radiations of the order

of 10^ times the power expected from the sun (assuming

that the sun behaves as a perfect blackbody radiator at a temperature of 6000°K) on Feb. 27 and 28, 1942, by radar

receiving equipment working at various wavelengths in the

4-6 m band. Evidence that the disturbance was caused by

electromagnetic radiations of solar origin was obtained by

the bearings and elevations measured independently by re- ceiving sets at widely separated points (Hull, Bristol,

Southampton, Yarmouth). It was determined that the noise

power received from the sun was of the order of 10"13 watt

per sq m per megacycle bandwidth. STRATTON states that

solar flares were observed on Feb. 21, 27, 28 and March 1,

at Mendon; a sudden fadeout on Feb. 28, and a magnetic

storm on March 1. The radio noise reported by HEY was

the earliest terrestrial phenomena observed preceding the

above events. (Met. Abst. 9A-6. )--M.L. R.

D-300 Hey, J. S. , Radio astronomy. Royal Astronomical Society,

Monthly Notices, 109(2): 179-214, 1949. 6 figs. , 3 tables,

numerous refs., 8 eqs. DLC--A progress report outlining

the fundamentals of radio transmission and reception in the

m and cm bands, and discussing technique and results in

the radar observation of meteor trails and of the moon, and

in the investigation of galactic and solar radio noise. A

full bibliography is appended. (Met. Abst. 9A-8. ) --Physics

Abstracts, No. 1388, 1950.

D-301 Hey, J. S. , Solar radio emissions at 4 metres wavelength

during 1947-50 inclusive, and their relation to solar activity. International Council of Scientific Unions. Commission for the Study of Solar and Terrestrial Relationships,

Rome, Sept. 1952, Proces -Verbal et Communications, pub.

1953. p. 16. DWB--Analysis of bursts of solar radio emission shows an average lag of a few minutes after solar

109
flares, but some bursts precede the flares. The average

order of occurrence of onset and maxima is set out. (Met.

Abst. 9A-36. )--C.E.P.B.

D-302 Hey, J. S. and Hughes, V.A. , Solar radio asymmetry at

4 metres wavelength. Nature, London, 173(4408): 771,

April 24, 1954. 3 refs. DWB-In 1948 HEY, PARSONS

and PHILLIPS found that bursts of radio emission on 4. 1

meters occurred more often associated with flares on east- ern than western half of the sun. In 1953 DODSON, HEDEMAN and OWREN did not find this effect on 1. 5 m. HEY

and HUGHES now point out that this result is to be expected

because absorption coefficient is proportional to 22 and the

difference may be still further increased by refraction. Asymmetry increased in 1950-51 when recurrent M-type magnetic

storms were becoming prominent, but observations had to

be discontinued in 1951. (Met. Abst. 9A-54. )--C.E.P. B.

D-303 Hey, J. S. (Radio Research Estab. , Malvern, England),

Solar radio eclipse observations . (In: Beer, Arthur, ed.

,

Vistas in astronomy. London, Pergamon Press, 1955. Vol.

1:521-531. 5 figs., 1 table, 28 refs., eq.) DLC (QB3.

B35)--The observation of the emission from the Sun at radio

wavelengths can provide knowledge of the localized regions

of bright radio emission and of the distribution of radio

brightness across the quiet Sun. From the latter it is possible to derive the distribution of electron density and temperature in the chromosphere and corona by measurement at

centimetre and metre wavelengths, respectively. Observations of solar radio emission at eclipses have been made

since 1945 and the results are discussed. (Met. Abst.

unpub. )- -Author's abstract.

D-304 Hibberd, F. H. (Cavendish Laboratories, Cambridge), The

effect of the ionosphere on the Doppler shift of radio signals

from an artificial satellite. Journal of Atmospheric and Terrestrial Physics, London, 12(4): 338-340, 1958. fig. , 5 eqs.

DLC --An idealized case of spherically stratified ionosphere

and a spherical earth is discussed with Snell's law applied

to the earth of a satellite emitted radio wave. (Met. Abst.

12. 7-125. )-W.N.

D-305 Hibberd, F. H. (Univ. New England, Armidale, N. S. W.

Australia), The Faraday fading of radio waves from an artificial satellite. Journal of Geophysical Research, Wash.

,

D.C., 64(8): 945-948, Aug. 1959. fig., 5 refs., 7 eqs.

DLC --Faraday fading of signals from an artificial satellite

is analyzed in terms of the difference between the Doppler

shifts of the ordinary and extraordinary components in the

110
ionosphere. A procedure is outlined for determining the

vertical distribution of electron density in the upper ionosphere. Explanations are given for the apparently excessive

values of electron content yielded by measurements of Faraday fading and for the observation that the rate of Faraday

fading is not exactly inversely proportional to the square of

the wave frequency. (Met. Abst. 11F-55. )--Author's abstract.

D-306 Hibberd, F. H. and Thomas, J. A. , The determination of

the electron distribution in the upper ionosphere from satellite Doppler observations . Journal of Atmospheric and Terrestrial Physics, N. Y. , 17(1/2):71-81, Dec. 1959. 7 figs.,

4 refs. , 15 eqs. DWB, DLC--It is shown how the electron

distribution in the upper regions of the ionosphere may be

determined from simultaneous measurements of the Doppler

shifts of radio signals of two different frequencies received

from an artificial satellite. The method is illustrated in detail by computations made on the 20 and 40 Mc/s signals

from Sputnik I. (Met. Abst. 11E-64. ) --Authors' abstract.

D-307 Hilton, W. F. (Hawker Siddeley Aviation, Great Britain),

A proposal for a British communications satellite. The New

Scientist, London, 8(203): 907 -909, Oct. 6, 1960. 5 figs.

DLC--Use of artificial satellites to receive a radio signal

from one part of the earth and relay it to another could be

extremely economical. With 90% launching success and a 22 yr life of a satellite the cost of transatlantic telephone

calls could be cut to one fortieth of the present cost. Wave

lengths of 300 Mc/s up to 11, 000 Mc/s could be used. A

discussion is given of the coverage that could be given by

various types of orbit. It is suggested that a system of

six satellites could give complete coverage over the whole

earth. A description is given of a suitable satellite which

would carry two radio transmitter-receivers each of 45 watts

radiofrequency power. Solar cells would be used to give a 500 watts d. c. electrical power. A method of stabilizing

the satellite so that the radio power could be directed as

required is suggested. There appears to be a good technical case for Britain to enter upon a program of design and

construction of a communications satellite. (Met. Abst.

12.7-77.)-R.B.

D-308 Hitchcock, R.J. ; Evans, G. O. and Naismith, R. , Sunspot-cycle variations in the discrepancies between predicted and observed frequencies for use in radio communication. Institution of Electrical Engineers, London, Proceedings,

Pt. B, 107(35) :423-426, Sept. I960. 6 figs. , foot-ref. DLC

(TK1. 14) --A marked variation occurs over the sunspot cycle

in the discrepancies between predicted F2-4000 km m. u. f.

Ill
and the observed times of fade-in and fade-out on an 18.4

Mc/s Bombay-London circuit. This is particularly marked

in summer and is attributed to the influence of the sporadic

E layer, although there is no marked sunspot-cycle effect

attributed to this layer. Any assessment of the accuracy

of predictions analyzed on the assumption of F layer propagation must be considered in relation to the phase of the

sunspot cycle to which it refers. (Met. Abst. 11L-245.

)

--Authors' abstract.

D-309 Hoffman, W.C. (Hughes Res. Lab., Malibu, Calif.),

A report on the symposium on the use of space vehicles at

the fall 1958. URSI meeting. Planetary and Space Science,

N.Y. , l(3):238-248, Aug. 1959. 13 figs. DWB-A symposium, under the chairmanship of A. H. Shapely, was held on

"The use of Space Vehicles" during the fall 1958 meeting at

Pennsylvania State University. Six others joined the panel.

The present paper briefly reports on the discussion and presents the pertinent graphical illustrations. The chairman,

in his opening remarks, reviewed the recent history of satellite radio experiments. The symposium was conducted on

the following plan: Five classes of experiments would be

discussed; a short five minute introduction for each type

being given by the panel members directly concerned, after

which the subject would be thrown open to discussion by

any interested member of the audience. The five classes

of experiments and the speakers for each were: (1) VLF

satellite measurements (R A.HELLIWELL and C. G. LITTLE).

(2) Ion probes (LC.SEDDON and MRS. SAGALYN). (3)

Faraday rotation measurements ( Co G. LITTLE and J. CSEDDON). (4) Topside ionospheric sounders (W.PFISTER and

O. GARRIOTT). (5) Studies of anomalous propagation

(W.PFISTER and O.GARRIOTT). (Met. Abst. unpub.)-

I.S.

D-310 Hood, Harold C. (Pacific Coast Editor), Spacemen may

communicate with gamma rays . Electronics, N. Y. , 35(2):

28-29, Jan. 12, 1962. 3 figs. DWB, DLC--J.E.Eersken

(Aerospace Corp.) predicts a jam-free space-to-space and

space-to-earth radio communication at around 10^-3 Mc/s

frequency, using gamma rays, a by-product from the nuclear

reactor powered satellites and space bases of the future.

(Met. Abst. unpub.)-W. N.

D-311 Hope, E. R. , Spiral patterning of solar corpuscular precipitation. Nature, London, 177(4508): 571-572, March 24,

1956. 2 figs. , table, 6 refs. DWB--Plots of radio blackout

distribution by G. m. t. agree with isochrons of 'morning'

maximum of magnetic disturbance in the Arctic. The Russian

112
isochrons (world time) and the isochrons of maximum percent

of blackout in summer (G. m. t. and 1. m. t. ) are shown and

discussed. (Met. Abst. 7. 8-112. )--C.E. P.B.

D-312 Horner, F. , Radio noise from planets. Nature, London,

180(4597): 1253, Dec. 7, 1957. 3 refs. DWB--J. D. KRAUS

suggested that high frequency radio noise received from

Jupiter and Venus may originate in discharges similar to

terrestrial lightning (Nature, 178:33, 1956). The author of

the present note compares amplitudes of sferics and of planetary radio noise and finds the latter to be considerably

larger than might be expected on the basis of KRAUS 's hypothesis. The discrepancy could be explained by larger

storm areas on the two planets and superposition of several

discharges. But before the hypothesis could be accepted

an explanation would have to be found for the fact that radio

noise from Venus and Jupiter is received in the form of

bursts rather than of continuous noise. (Met. Abst. 9A154.)-G.T.

D-313 Houston, R.E. , Jr. ; Ross, W.J. and Schmerling, E. R.

,

Some effects of intense solar activity on radio propagation. Journal of Atmospherics and Terrestrial Physics, 10(3):136-

139, March 1957. 4 figs. , 2 refs. DWB--Observations on

75 kc/s at vertical incidence at Ionosphere Research Lab.

(Pa. ) during solar flare of 0300 UT on Feb. 23, 1956, are

reported. No significant change of group height was noted.

Phase height showed a rapid decrease of 8 km beginning

2238 + 3 LMST and lasting an hour. A large increase of

absorption occurred 15 min after visual observation of the

solar event. (Met. Abst. 10. 4-156. )-C.E. P. B.

D-314 Hoyle, Fred, Some recent researches in solar physics . Cambridge, England, University Press, 1949. 134 p. 8

figs., 36 tables, refs., 2 append. (Cambridge Monographs

on Physics) MH-BH, DLC--A technical treatise intended

for the astrophysicist and concerned mainly with the theoretical aspects of solar physics and solar terrestrial relationships. Separate chapters include a discussion of: (1)

sun spots and the solar cycle (11 yrs), (2) observational

data and (3 & 4) theory of the chromosphere and corona,

(5) the magnetic field and convective circulation of the sun,

(6) terrestrial magnetic storms, the aurora and the earth's

ionosphere, and finally, (7) the emission of radio waves

from the sun. Appendices and supplementary notes include

material on nomenclature and symbols, the origin of the

solar magnetic field and the aurora. (Met. Abst. 2. 1-94.

)

--M.R.

113
D-315 Huang, Chun-Ming (Radio Wave Res. Lab., Taipei, China),

Some abnormalities in the variations of F2 layer critical

frequency during the period of high solar activity of solar

cycle 8-19. Journal of Geophysical Research, Wash. , D.C.,

65(3):897-906, March 1960. 16 figs. , 2 tables. DLC--

Some abnormalities in the variations of foF2 were observed

at Taipei during the period of very high solar activity of

solar cycle 8-19. They are the saturation effect of foF2

(i. e. , the increasing rate of foF2 with respect to sunspot

number is nearly zero at high solar activity), the occurrence of post-sunset peak of foF2, and the increase of

foF2 during the ring eclipse. In this report variations of

these phenomena are described, the close relationship existing among them is examined, and a probable explanation

is given. (Met. Abst. 11. 10-152. ) --Author's abstract.

D-316 Huang, Su-Shu (Institute for Advanced Study, Princeton,

N. J. ), Some astronomical aspects of life in the universe . Sky and Telescope, 21(6):312-316, June 1961. 6 figs.

,

2 tables. --Only through radio communication may the possibly existing extraterrestrial and intelligent beings be

reached. The frequency of the 21 cm neutral hydrogen line

may be used to establish contact by means of codes suggested. Author believes that "no more than one or two percent of stars may have at one time or another supported intelligent life. " Our neighbor stars, Tau Ceti and Epsilon

Eridani, satisfy his criteria for possible existing civilizations. --W. N.

D-317 Huber, P. W. (NASA, Wash., D.C.), Experiments with

plasmas produced by alkali metal seeded cyanogen-oxygen

flames for study of electromagnetic wave propagation at the

Langley Research Center. Planetary and Space Science,

N.Y. , 6:172-179, June 1961. 15 figs., 3 refs. DWB--This

article gives the status of the work done at the Langley Research Center of the National Aeronautics and Space Administration. Methods and equipment to study the topic, both

theoretically and experimentally, are designed to comprehend the mechanisms of the interactions within the plasma

layer and the electromagnetic wave. The utility of the

alkali seeded cyanogen-oxygen flame to produce controlable

conditions is reflected in the successful results obtained.

--W. N.

D-318 Hultqvist, Bengt, On the interpretation of ionization in the

lower ionosphere occurring on both day and night side of the

earth within a few hours after some solar flare. Tellus,

ll(3):332-343, Aug. 1959. 9 figs. , 3 tables, 23 refs. , 6

eqs. DLC--The absorption effect following solar flares may

114
be interpreted as being caused by a high energy ion beam

of very small density emitted from the sun, the ions moving

in Stormer orbits. -IRE Abst. 2374

D-319 Hultqvist, B. and Ortner, Johannes (both, Kiruna Geophysical Obs. , Sweden), Observations of intense ionization

of long duration below 50 km altitude after some strong

solar flares . Nature, London, 183(4669): 1179-1180, April

25, 1959. fig. , 7 refs. DWB-On July 7 and Aug. 16, 22

and 26, 1958, very strong absorption was measured with

C.G. LITTLE'S riometer (relative ionospheric opacity meter)

at Kiruna Geophysical Observatory, Sweden. The observation succeeded the outbreak of 3+ solar flares by a few

hours. The maximum daytime absorption was 15 db in

three of the cases. The results are presented in facsimile

riometer recordings and discussed in support of the hypothesis that the ionizing agent was sun-emitted protons from the

flares. (Met. Abst. 11D-60. )--N. N.

D-320 Hund, August, Short wave radiation phenomena. 1st ed.

New York, McGraw-Hill, 1952. 2nd vol. (1332 p.). 394

figs., 97 tables, 1009 eqs., bibliog. p. 1288-1301. DLC--

This valuable work covers theoretical and experimental contributions from the discovery of the electromagnetic wave

to their applications in radio communication and in guided

missiles. In its two volumes, the nine chapters are broken

down in sections under Subject Headings: Chapter (1) Fundamental concepts and relations of currents and electromagnetic fields; (2) Space electromagnetic fields of elementary

electric and magnetic dipoles; (3) Fundamental methods

used in electromagnetic theory; (4) Propagation characteristics; (5) Transmission lines and radiation; (6) Unobstructed space radiation; (7) Space radiation in the presence of electromagnetic obstruction; (8) Electromagnetic

diffraction; and (9) Wave guides and cavities. Cross references are provided. The three last chapters are particularly of radio-meteorological interest. The appendix provides a list of the symbols used and an extensive bibliography. (Met. Abst. 4. 4-278.) --W.N.

D-321 Huntley, H. E. , Radio astronomy in the tropics. Nature,

London, 172(4368): 108, July 18, 1953. ref. DWB--Account

of a radio-astronomy observatory at Achimota, near Accra,

Gold Coast, started Jan. 1952. Program includes hour-byhour recordings of F layer disturbances, solar activity and

coordinates of radio stars. (Met. Abst. 4. 11-38. )--C.E. P. B.

115
D-322 Hutchinson, H. P. and Arendt, P. R. , Ionospheric scintillations of satellite signals. Institute of Radio Engineers, N. Y.,

Proceedings, 48(4):670-S71, April 1960. 7 figs. , ref. DLC--

The scintillation of satellite emitted radio signals has been

observed using two different techniques, namely, Doppler

shift frequency measurements and radio direction finding. In

this shortened version of a more complete paper, there are given the results obtained using Doppler shift measurements

only. Variations from a smooth Doppler shift curve obtained

during individual orbits give a measure of the frequency scintillation occurring and thus of the roughness of the ionospheric path between the satellite and the observer. As ex- pected, these variations are a function of frequency, and

they become less as the frequency is increased. (Met. Abst.

11. 12-371. )--Authors' abstract.

D-323 Huxley, L.G.H. (Univ. of Adelaide), A discussion of the

motion in nitrogen of free electrons with small energies with

reference to the ionosphere. Journal of Atmospheric and Terrestrial Physics, N. Y. , 12(l/2):46-58, Oct. 1959. 4 tables,

6 refs. , 28 eqs. DWB, DLC--In this paper measurements of

diffusion and drift of slow electrons in pure nitrogen carried

out by Crompton and Hall, are discussed. The discussion is

restricted to the range of energies of the electrons between

that of thermal equilibrium and four times that value. From

the behavior of the coefficient of diffusion D it is concluded

that in elastic collisions between electrons and nitrogen

molecules, the collisional cross section A is proportional to

the speed c of the electron; namely, A - 3. 29 X 10"^3 c cm^ . From this result an accurate expression is derivable

for the velocity of drift W in terms of the parameter Z/P and

the mean energy of agitation of the electron. The measured

rate W at which electrons with energy Q lose energy in collisions with molecules is accurately described by a formula

that ascribes these losses of energy chiefly to the excitation

of changes in the rotational states of the molecules. A

formula in close agreement with the measurements is derived

for the dependence of the mean energy of agitation of the

electrons upon Z/P. The significance of the measurements

for ionospheric studies is considered with particular reference to the interpretation of measurements of radio wave interactidn. It is shown that the values of the molecular concentration in the height range 82 to 90 km above the ground,

found by means of radio wave interaction, are consistent

with the A. R. D.C. model atmosphere ( MINZER and RIPLEY,

1956). (Met. Abst. 11D-63. ) -Author's abstract.

116
D-324 Hyde, Margaret O. , Exploring earth and space: the story

of the I. G. Y. Illus. by Clifford N. Geary. N. Y. , Whittlesey House, 1957. 160 p. DLC (QC801. 3. H9)--A readable and accurate account of the IGY and its various phases

including chapters on earthquakes, volcanoes, the Antarctic,

oceanographic research, weather control; atomic, cosmic and

solar energy or applications; rockets, satellites and radioastronomy; the airglow, aurora, balloons (manned and with

animals or pilot radio and instruments). Geomagnetism,

gravity, climatic changes, the ionosphere, glaciers, tidal

waves, etc. , are treated incidentally. (Met. Abst. 9. 4-24. ) --M.R.

D-325 Ikhsanov, R.N. (Main Astronom. Obs.,Acad. Sciences,

USSR), On the nature of Cvo I. Soviet Astronomy AJ, N. Y.,

4(6):923-928, May/June 1961. fig., 2 tables, 16 refs. , 2

eqs. DLC. Transl. of original Russian in Astronomicheskii

Zhurnal, Moscow, 37(6): 988-993, Nov. /Dec. 1960. DLC--

The absorption in the path from radio sources is determined

on the basis of a simultaneous analysis of radio and optical

data. The distance to the sources is determined and the physical possibility of their existence at such distances is discussed. It is shown that at least an appreciable fraction of

radio emission of the principal component of Cyg I is due to

the emission of the nebula associated with IC 1318. (Met.

Abst. unpub. ) --Author's abstract.

D-326 Ingalls, R.P. ; James, J.C. and Stone, M.L. (all, MIT,

Lincoln Lab. ), Study of UHF space communications through

an aurora using the Moon as a reflector. Planetary and Space

Science, N. Y. , 7:272-285, July 1961. 11 figs. , 15 refs.

DWB, DLC --Lunar CW transmissions from College, Alaska,

were received at Millstone Site, Westford, Mass. , and at

Shirley Bay site, near Ottawa, Ontario, where identical re- ceivers were used. Every one-half hour lunar transmissions,

at 440 Mc/s, were conducted for 20 min and during the re- maining 10 min a radar search at 398 Mc/s was made; the

equipment calibration was checked at the receiving sites.

The results presented in graphs show the effects of a quiet

and an aurorally disturbed ionosphere on the propagation of

UHF signals into space. Also confirms and extends earlier

results of moon reflection characteristics. --W. N.

D-327 Inoue, Yuji (Tech. Res. Inst. , Nat'l. Defense Agency,

Tokyo), On the importance of the resonance lines of atomic

oxygen to the ionospheric ionization. Journal of Atmospheric

and Terrestrial Physics, London, 15(1/2): 85-88, Sept. 1959.

eqs. DLC--A new interpretation of the effective recombination coefficients of an electron in the ionosphere is advocated. A new theory for the ionization mechanism in the

117
ionosphere is also brought forward. The resonance lines of

atomic oxygen are of 1302 - 1306 A, 3 s — 2 p , and

3 D

° 3P

1025. 7 A, 3d -2 p , These lines were observed

at 115 km as a strong emission. The new theories of the

ionosphere are discussed, relating to the interpretation of

the formation of these emission lines in the ionosphere.

(Met. Abst. 11. 9-118.)- -Author's abstract.

D-328 International Geophysical Year, 1957/1958. IGY World

Data Center A (for) Solar Activity, High Altitude Observatory, Boulder, Colo. , Intermediate reports of surges and active prominence regions, Oct. -Dec. 1958. Its IGY Solar Activity Report Series, No. 7, June 1, 1959. unpaged (1 p. per

day). Entirely tables. Also Jan. -March 1959. Ibid., No. 8,

Sept. 1, 1959. unpaged. Entirely tables. Also April -June

1959. Ibid. , No. 9, Feb. 22, 1960. unpaged. Entirely

tables. DWB (523. 74 1612s o) -These are the original, un- corrected data compiled from the daily reports of various observations during the period Oct. 1958 to June 1959. (Met.

Abst. 11. 9-74.) -N.N.

D-329 International Geophysical Year, 1957/58. Japanese National

Committee for the IGY, Compilation of data in Japan for atmospheric radio noise during the International Geophysical

Year 1957/58. Ueno Park, Tokyo, Japan, National Committee

of the IGY, Science Council of Japan, March 1960. 156 p.

figs., tables. DWB (551. C6 I13ja)--A compilation of atmospheric radio noise data which includes tables and curves of

noise level values and cumulative amplitude distribution

curves for the period Sept. 18, 1957 to Dec. 17, 1958. Brief

notes explain the distribution of stations, methods and schedules. Block diagrams of apparatus and symbols used are included. The data were collected in Japan during the International Geophysical Year. (Met. Abst. 13. l-46.)--E.'Z.S.

D-330 International Scientific Radio Union, 11th General Assembly,

The Hague, Aug. 23-Sept. 2, 1954, Proceedings, Vol. 10.

Pt. 5, Commission No. 5 on Radio Astronomy, 1955? 113 p.

tables, refs. DWB--Members hip of the Commission on Radio

Astronomy and subcommissions (Solar Radio Emissions, Terminology, Basic Solar Index and Standardization of Equipment

and Measurements), a list of 27 reports and papers submitted,

reports of subcommissions, reports of national committees of

Australia, Canada, Finland, France, Germany, Great Britain,

Italy, Japan, Netherlands, Spain, Sweden, Switzerland and

U.S., address of M.LAFFINEUR, President, minutes of sessions, etc. , are included in report along with numerous references to literature published in each country. (Met. Abst.

9A-57. )-M. R.

118
D-331 International Telecommunication Union, Revision des donnees sur les bruits atmospheriques radioelectrigues . (Revision of the data on the atmospheric radio-electric noises.)

Prepared by the International Radio Consultative Committee

(and its Report No. 65, issued Geneva, 1957. ) 34 p. 27

figs. , 14 refs. --In preparing this report, a greater account

was taken of the data gathered during a period of great solar

activity than of those relative to a period of weak solar activity. In spite of the reasons which allow us to believe that

the phase of the solar cycle will have an influence on the

degree of the noise at its reception, it has not been possible

to put into evidence a satisfying correlation between the sunspots and the data available on the noise. As often as possible, the forecasts are based on actual measurements. The

report deals successively with basis parameters, graphically

represented parameters, factors intervening in forecasts,

variations in the degree of the noise within a section, fine

structure of the atmospheric noise and use of the data. (Met.

Abst. 10D-59.)-A.V.

D-332 Israel, Hans, Sonne und Erde. (Sun and earth. ) Naturwissenschaftliche Rundschau, 3(3):101-106, March 1950. 8 figs.

DWB--The source of solar energy, its effect on the upper atmosphere and on radio transmission and the possible relationship between sunspots and weather are discussed and illustrated. The spectral distribution of energy at different heights,

ionization in different regions of the ionosphere and the relation of sunspots to rainfall, tree rings and the height of Lake

Victoria are among the illustrations presented. (Met. Abst.

2.4-60.)--M. R.

D-333 Istomin, V. G. , Radiochastotnyi mass-spektrometr dlia is - sledovanii ionnoqo sostava verkhnei atmosfery. (Radio frequency mass spectrometer for investigating the ion content

of the upper atmosphere. ) Iskusstvennye Sputniki Zemli,

Moscow, No. 3:98-112, 1959. 15 figs. , 19 refs. DLC, DWB.

Summary in U.S. National Aeronautics and Space Administration, Technical Translations, F-8:9, April 1960. Complete

transl. to be issued in the Technical Translations series. •- Detailed description of the radio frequency mass spectrometer

used to determine the ionic composition of upper atmosphere.

Data on the mass spectrum of positive ions in the ionosphere

at an altitude up to 855 km were obtained from Sputnik III and

from high altitude rockets. The mass determination range of

the device is from 6-48 atomic mass units and the scanning

time for the whole range is 1. 7 sec. (Met. Abst. 11. 12-373.

--E. K.

119
D-334 Iwai, Akira and Outsu, Jinsuke, On an investigation of

whistling atmospherics in Japan. Nagoya. Univ. Research

Institute of Atmospherics, Proceedings, 4:29-47, Dec. 1956.

17 figs. , 3 tables, 9 refs. , eqs. DWB--As part of the Study

Program of I. G. Y. , we have prepared an observation of whistling atmospherics. Since Jan. 1956, continuous observations

of whistlers have been made at Toyokawa (geomag. lat. 24. 5 ). Simultaneous observations at Toyokawa and Wakkanai (geomag.

lat. 35. 3 ) were made for one month beginning July 13, 1956.

The results obtained in the analysis of the dispersion of whistlers were essentially similar to those reported by STOREY.

But, at Toyokawa, long whistlers, whistler trains and whistler pairs have not been observed, only short whistlers being

observed. The greater part of the observed whistlers occurred

in winter; in other seasons it was scarcely possible to detect

them. At Wakkanai, long whistlers and whistler pairs have

been observed this summer, but whistler trains have not been

observed during this period. (Met. Abst. 9. 4-282. ) --Authors'

abstract.

D-335 Iwanowska, IVilhelmina, Fale radiowe pochodzenia kosmicznego. (Radio waves of cosmic source. ) Przeglad Meteorologiczny i Hydrologiczny, Warsaw, No. 2-4:3-10, Dec. 1948.

fig. English summary p. 10. DWB--The entire spectrum of

radiation from the ultraviolet to the long wave radio frequencies (10"* to 10^ cm) is shown graphically and a general discussion of theories as to their origin (solar and cosmic) and

the influence of magnetic fields of sun and earth thereon, included. The relation of sunspots and other factors to radio

emissions is also reviewed. (Met. Abst. 2. 7-182. )--M. R.

D-336 Jacchia, L. G. , Solar effects on the acceleration of artificial

satellites. Smithsonian Institution. Astrophysical Observatory, Special Report No. 29, Sept. 21, 1959. 15 p. 4 figs.,

2 tables, 8 refs. DWB--Four types of fluctuations are described and explained. Those following the rhythm of the solar

flux at 2800 Mc probably reflect variations in atmospheric

density caused by variable short wave solar radiation. A

slow fluctuation connected with the position of the perigee

with respect to the sub-polar, reflects a difference in the density profiles of the bright and dark hemispheres of the earth.

Transient fluctuations accompanying magnetic storms should

reflect a heating of the atmosphere through some interaction

with corpuscular radiation. Erratic fluctuations of unexplained origin indicate a connection with conditions in the radiation belts. The diagrams illustrate the correspondence of the

different accelerations by each solar disturbance. The secular accelerations for three satellites, as well as relative positions of sun and perigee for them, are shown in tables. (Met.

Abst. 11. 12-550. )--O.T.

120
D-337 Jackson, J.E. , Effect of oblique propagation paths upon the

NRL rocket studies of the ionosphere. U. S. Naval Research

Laboratory,. NRL Report, 4960, July 23, 1957. 15 p. 7 figs.,

3 tables, 7 refs. (Upper Atmosphere Research Report, No.

29). DWB (Mil U58u) --Results of ten years of vertical propagation tests from signals emitted by rockets are reviewed

and the anomalous conditions discovered when paths were

inadvertently oblique, discussed in detail. Effects due to

the earth's magnetic field, to reflected rays and rocket roll are considered for the vertical case and effects due to bending of rays considered for the oblique case, as exemplified

by the flight of Aerobee-Hi-NRL-50. The corrections for electron densities as calculated from this oblique case are also

treated. These corrections are 1) for changing electron density along successive propagation paths, and 2) variation in

angle between propagation path and geomagnetic field (near

peak of path). (Met. Abst. 12. 4-129. )--M. R.

D-338 Jacobs, George (Dept. Editor, CQ), DX and the sun. Pt. 1-

2. CQ, Radio Amateur's Journal, N. Y. , 9(7): 15-18, 60-61,

July 1953 and 9(8):20-21, 59, Aug. 1953. 7 figs. , photo.

DWB--This article has been written for the "DX-hound", the

radio amateur ever eager to pick up a station from Distance

X (the greatest possible distance) over high frequency ionospheric radio communication. Pt. I gives basic knowledge on

sunspot cycles and ionospheric conditions and on their effect on radio propagation. Diagrams showing past and present sunspot cycles and correlation between sunspot numbers

and critical frequencies are presented. Daily and seasonal

solar variations and their effects are also discussed and illustrated. Pt. II explains the role of the ionosphere in absorption of radio waves of varying length and the effect of solar

activity on this absorption; a forecast of general propagation conditions is given for 1953-56. (Met. Abst. 6D-182.

)

--G.T., M.R.

D-339 Jansky, Karl Guthe, Directional studies of atmospherics at

high frequencies. Institute of Radio Engineers, N. Y. , Proceedings, 20(12): 1920-1932, Dec. 1932. 14 figs., table,

6 refs. DLC --Describes a series of experiments as conducted

at Holmdel, N. J. , from Aug. 1931 in order to study the direction of arrival and the intensity of static using a 14. 6 m radio

system, which is illustrated and described in block diagrams.

Three distinct groups of static were recorded: 1) From local

thunderstorms; 2) from the Heaviside layer; and 3) from un- known source. The latter with an intensity "^='0.39 microvolt

per meter for 1 Kc band width. Apparently this static is as- sociated somehow with the sun. Closer studies are required.

--W. N.

121
D-340 Jansky, K. G. , Radio waves from outside the solar system.

Nature, London, 132(3323):66, July 8, 1933. ref. DLC--

Based on new records the author found that the source of

static is a region stationary with respect to the stars, the

right ascension of this region is established within + 30 min.

Mention is made to the earlier assumption (1932) that the

source of static was somehow associated with the sun which

was disproved. --W. N.

D-341 Jansky, K. G. , Electrical disturbances apparently of extra - terrestrial origin. Institute of Radio Engineers, N. Y. , Proceedings, 21(10): 1387-1398, Oct. 1933. 9 figs. , 3 refs.

DLC --Electromagnetic waves of an unknown origin were detected during a series of experiments on atmospherics at

high frequencies. Directional records have been taken of

these waves for a period of over a year. The data obtained

from these records show that the horizontal component of

the direction of arrival changes approximately 360 in about

24 hrs in a manner that is accounted for by the daily rotation

of the earth. Furthermore, the time at which these waves

are a maximum and the direction from which they come at

that time changes gradually throughout the year in a way

that is accounted for by the rotation of the earth about the sun. These facts lead to the conclusion that the direction

of arrival of these waves is fixed in space; i. e. , that the

waves come from some source outside the solar system. Although the right ascension of this source can be determined

from the data with considerable accuracy, the error not being

greater than + 7.5 , the limitations of the apparatus and the

errors that might be caused by the ionized layers of the

earth's atmosphere and by the attenuation of the waves in

passing over the surface of the earth are such that the declination of the source can be determined only approximately.

Thus the value obtained might be in error by as much as ±30 . The data given for the coordinates of the region from which

the waves seem to come show a right ascension of 18 hrs and

a declination of —10 . (Met. Abst. 9A-1. )--Author's abstract.

D-342 Jansky, K. G. , A note on the source of interstellar interference. Institute of Radio Engineers, N. Y. , Proceedings,

23(10):1158-1163, Oct. 1935. 2 figs. , 4 refs. DLC--Enhanced radiation energy was observed whenever the antenna

was directed at the Milky Way, perhaps because of the greater star density. Another plausible explanation is that the en- hanced radiation is due to secondary radiation caused by high

speed particle bombardment from the stars. --W. N.

122
D-343 Jansky, K. G. , Minimum noise level obtained on short wave

radio receiving; systems . Institute of Radio Engineers, N. Y. , Proceedings, 25(12): 1517-1530, Dec. 1937. 13 figs., 15 refs.

DLC --Experiments with radio equipment developed at the Holmdel Radio Laboratories, New Jersey, of Bell Telephone Laboratories Inc. , are described. The purpose was to check the

noise level in absence of atmospheric and man made interference on radio communication. The extraterrestrial noise observed on 14 m, 16. 7 m, and on 32. 2 m comes from the Milky

Way. -W. N.

D-344 Jansky, C. M. , Jr. , The beginnings of radio astronomy.

American Scientist, New Haven, Conn. , 45(1):5-12, Jan.

1957. photo. DLC -A biography of KARL GUTHE JANSKY

(1905-1950). Recounts briefly family history, his brother's

education and circumstances under which he became an employee of the Bell Telephone Laboratories in 1928. Reviews

KARL JANSKY's work from 1928-1932 which led to the discovery which furnished the foundation for the science of

radio astronomy. Closes with the statement that KARL JANSKY's "philosophy of life was that of a true scientist - perserverence, the accumulation of data, objectivity in analysis, modesty, credit to others for their contributions, and a willingness to leave the ultimate evaluation of one's work to

the future/' (Met. Abst. 9A-167. )--M.L. R.

D-345 Jansky, C. M. , Jr. , The discovery and identification by Karl

Guthe Jansky of electromagnetic radiation of extraterrestrial

origin in the radio spectrum. Institute of Radio Engineers,

N. Y. , Proceedings, 46(1):13-15, Jan. 1958. 2 refs. DLC--

December 1957 marks the 25th anniversary of the completion

of Karl Guthe Jansky's field studies which proved that electromagnetic waves in the radio spectrum of extraterrestrial

origin were reaching the earth. April 1958 will mark the 25th

anniversary of the date on which this basic discovery was

disclosed in full to the scientific world. This paper describ- es briefly the steps which led to Jansky's basic discovery,

some of the important results of later studies in radio astronomy, and the relationship between pure and applied science

illustrated by the basic discovery and subsequent work in

this field. (Met. Abst. unpub. )- -Author's abstract.

D-346 Japan. Science Council. Ionosphere Research Committee,

Catalogue of disturbances in ionosphere, geomagnetic field,

field intensity of radio wave, cosmic ray, solar phenomena

and other related phenomena. No. 10. the 31st cooperative

observation. June 10-July 10. 1951. (1951?) 39 p. graphs,

tables. DWB--This observation period is especially interesting owing to a great solar eruption with two severe magnetic storms and a conspicuous decrease of cosmic ray intensity.

123
A photo of the eruption is added and the observation results

are presented in numerous graphs and tables. (Met. Abst.

6D-71.)--A.A.

D-347 Jasik, Henry (JasikLabs., Westbury, N. Y. ), A wide band

antenna system for solar noise studies. Institute of Radio

Engineers, N. Y. , Proceedings, 46(1): 135-142, Jan. 1958.

11 figs. DLC--A wide band antenna system has been developed as part of a sweep frequency spectrum analyzer for solar

noise studies in the 100 mc to 600 mc frequency range. The

antenna system consists of an equatorially mounted 28 ft paraboloid illuminated by a unique feed combination which

operates over the frequency range in three over-lapping bands.

Development of the antenna system has been carried out with

the aid of scale models and two full size systems have been

constructed. The resulting antenna has an effective area

which is reasonably constant over the entire range before re- flection losses are considered. The feed configuration is

described and performance characteristics are given. (Met.

Abst. 11. 8-54. )--Author's abstract.

D-348 Jaye, W.E. ; Dyce, R.B. and Leadabrand, R.L. (all, Stanford Res. Inst. Menlo Park, Calif.), Radar echoes obtained

from Earth satellites' 1957 Alpha and 1957 Beta. Planetary

and Space Science, N. Y. , 5(l):50-58, Jan. 1961. 7 figs.

,

7 refs. , 2 eqs. DWB--On 16 occasions, radar echoes were

obtained from the first Russian earth satellite, 1957 Alpha,

by allowing the satellite to pass through the antenna beam,

which was aimed at the point of closest approach. Fortyeight echoes were obtained from 1957 Beta, the largest apparent cross section being 437 m^. A median cross section

of 1. 8 m^ was obtained. The echo exhibited a cyclic amplitude fluctuation which was observed to be as low as 0. 1 c/s

and as fast as 0.9 c/s. Although calculations indicate that

ionospheric Faraday rotation was present in many cases, the

amplitude fluctuation of the back scattered echo generally

prevented its identification. One occasion is reported of a

rapid, irregular amplitude fluctuation imposed on the echo

by aurora. (Met. Abst. unpub. ) --Authors' abstract.

D-349 Jelley, J. V., Cerenkov radiation and its applications. Published for the United Kingdom Atomic Energy Authority. N. Y.,

Pergamon Press, 1958. 304 p. figs. , tables, bibliog. (p.

289-296), eqs. Price: $10. 00. DWB, DLC (QC475.J42).

Review by E. P. Kincks in Science, Wash. , D. C. , 129(3358):

1273, May 8, 1959. --The first thorough review in book form

of the theoretical, experimental and applied aspects of this

peculiar form of radiation named Cerenkov radiation after its

discoverer. The field is narrow but touches on nuclear physics, optics, high frequency radio techniques, astrophysics

124
and cosmic rays. The faint, bluish-white light, given off

by transparent objects in proximity to radioactive sources,

was first noticed in 1910 by MADAM CURIE, was studied

by L. MALLET in 1926-1929, but was not identified and ex- plained until 1934-1938. Applications to measurement of

speed of high energy particles, night airglow, cosmic rays,

etc. , arose from the use of the photomultiplier and the re- sulting scintillation counter. Generation of microwaves by

Cerenkov radiation is also considered. The photomultiplier

and Cerenkov detectors are treated in detail. Optical considerations, design of counters, Cerenkov radiation in the

atmosphere, gas counters and miscellaneous aspects are treated in several chapters. Light pulses from the night sky

were discovered during cosmic ray shower in 1953. (Met.

Abst. llB-65.)--M.R.

D-350 Jplley, J. V. (Atomic Energy Res. Estab. , Harwell, Eng. ), Cerenkov radiation in the atmosphere. Planetary and Space

Science, N. Y. , 1(2):1Q5-111, April 1959. 4 figs., table,

18 refs. , 6 eqs. DWB--The bursts of large numbers of electrons produced in the atmosphere by cosmic ray air shfcwers

give rise to Cere-kov radiation in the air. The showers are,

therefore, accompanied by light pulses of short duration;

these may be detected quite easily with simple apparatus on

a clear dark night. This phenomenon, which was discovered

by the author and his colleagues in England in 1953, has

been studied in more detail by two groups, one in the U.S.

S. R. and one in Australia. In this article, the writer re- views the theoretical and experimental work that has been

done up to the present time, and discusses the potentialities and limitations of the technique as a new tool for cosmic ray research. The paper concludes with a few remarks

on the future possibilities in this field, and the likely technical developments. (Met. Abst. 11. 2-198. )--Author's abstract.

D-351 Jennison, R.C., The radio exploration of space. British

Interplanetary Society, Journal, 14(6): 307 -314, Nov. /Dec.

1955. DLC--The general principles and applications of radio

astronomy are outlined, and reference is made to the various

types of radio telescopes in use at present. A short account

is given of the detection of meteor activity, the aurora, and

the moon by radar techniques; the remainder of the paper describes the various aspects of radio astronomy associated with

the emission of radio noise. (Met. Abst. 9A-77. ) --Author's

abstract.

125
D-352 Jermison, R.C. (Nuffield Radio Astronomy Obs. , Jodrell

Bank), Radio astronomy from artificial satellites . The New

Scientist, London, 8(211): 1450-1452, Dec. 1, 1960. 4 figs.

--The part of the spectrum from which extraterrestrial signals

are observable at the earth's surface is limited. Very little

is known about the spectrum of frequencies below about 15

Mc/s. Observations from satellites in these frequency bands

have not yet been made because of the difficulties of producing a sufficiently large aerial. A solution to this problem

would'be the use of long lengths of conducting material in

the form of a sprung coil of concave section which could disgorge itself rapidly to form a long straight conducting element. An alternative would be wires mounted on reels with

weights at their ends which, when released, would extend

straight outward under the action of centrifugal force. --R.B.

D-353 Johnson, Francis S. (Lockheed Aircraft Corp. , Palo Alto,

Calif. ), Temperatures in the high atmosphere. Annales de

Geophysique, Paris, 14(1):94-108, Jan. /March 1958. 11

figs., 15 refs. French and English summaries p. 94. DLC--

The temperature distribution of the high atmosphere is discussed on the assumption that the ionosphere is heated primarily by solar radiation and that the temperature distribution is controlled by thermal conduction. A model is presented which agrees well with the rocket observations and

with most of the radio observations, and in which the thermal conduction is consistent with the absorption of solar

energy. The amounts of solar energy are in agreement with

the rocket observations in those spectral regions in which

observations have been made. However, no observations

have been made in the spectral region which is most important with regard to controlling the temperature of the F re- gion of the ionosphere. The amount of solar energy which

must be assumed to be present in this spectral region in

order to give a thermally consistent model with temperatures as high as those required by rocket and radio observations is not unreasonable from an astrophysical viewpoint. (Met. Abst. 12E-115. )--Author's abstract.

D-354 Johnson, F.S. (Lockheed Missiles and Space Div. , Calif.),

The exosphere and upper F region. Journal of Geophysical

Research, Wash., D.C., 65(9): 2571 -2575, Sept. 1960. 4

figs. , 19 refs. DLC--The view is presented that the outer

portion of the earth's ionosphere, through which radio whistlers propagate, has its origin in the earth's atmosphere rather

than in interplanetary space. The outer portion of the earth's

neutral particle exosphere is dominated by neutral atomic

hydrogen which is escaping steadily from the earth's atmosphere. Some of this neutral atomic hydrogen reacts with

126
atomic oxygen ions near the base of the exosphere, giving

rise to hydrogen ions. Diffusive equilibrium is the dominant factor controlling the relative concentration of ions and

neutral particles near the base of the exosphere. At higher

levels, the geomagnetic field exerts an influence in that it causes the ions and electrons to rotate with the earth, and

the centrifugal force modifies the force of gravitational attraction appreciably. The ion electron plasma through which

the radio whistlers propagate is hydrostatically supported

within the magnetic tubes of force. (Met. Abst. 11. 12-400. ) --Author's abstract.

D-355 Johnson, F. S. (ed. ) (Lockheed Aircraft Corp. , Palo Alto,

Calif. ), Satellite environment handbook. Stanford, Calif.

Stanford Univ. Press, 1961. 155 p. figs. , tables, eqs.

refs. at end of each chapter. DLC--This handbook contains

a comprehensive summary of available data describing the

geophysical environment encountered by artificial Earth satellites. The major satellite environment factors, the structure of the upper atmosphere and the ionosphere, penetrating

particle radiation, solar radiation, micrometeorites, radio

noise, thermal radiation from Earth, and geomagnetism are discussed, and existing data are evaluated. The various

known sources of the penetrating radiations found in space

are summarized by type of radiation, flux, particle energy.

Comments and references for each type are included. The

following supplementary data are included in the appendix:

solar system data; earth satellites and space probes to

April 24, 1961; conversion factors; and useful physical

constants. (Met. Abst. unpub. )--E. Z. S.

D-356 Johnson, M.H. (Rad. Lab., Univ. of Calif. ), The connection between lunar height changes and lunar currents in the

E layer. Journal of Geophysical Research, 59(2):247-251,

June 1954. 4 refs. , 15 eqs. MH-BH--The height changes

produced by vertical electronic diffusion in the presence cf

negative ions are examined in some detail. Application of

the results to the E layer shows that a previous qualitative

discussion remains valid. (Met. Abst. 6D-247. )—Author's

abstract.

D-357 Jones, I.L. (Cavendish Lab. , Cambridge), Further observations of radio stellar scintillation. Journal of Atmospheric

and Terrestrial Physics, London, 19(l):26-36, Sept. 1960.

6 figs. , 17 refs. DLC- -Observations are described of the

scintillation of the radio signal received from the radio star

in Cassiopeia on a frequency of 38 Mc/s. Further experimental results are presented to support SPENCER 's (1955)

evidence that the irregularities responsible for the radio

stellar scintillation are elongated with their long axes along

127
the lines of force of the earth's magnetic field. An estimate of the size of the irregularities in the ionosphere is

made, and a marked decrease in the long axis of the irregularities is found as the elevation of the radio source decreases. Evidence is put forward which suggests that turbulence is unimportant on most occasions in the region re- sponsible for the scintillation. (Met. Abst. 11.12-34.)--

Author's abstract.

D-358 Jones, Robert E. , Ionosphere research. Pennsylvania.

State College, Ionosphere Research Laboratory, Contract

AF 19(122)-44, Final Report, March 25, 1949-Jan. 31, 1955.

Jan. 31, 1955. 105 p. bibliog. Mimeo. DWB--Over 200

reports and scientific papers, which have emanated from

this project in 5^ yrs, are listed and abstracts given on all

of the scientific reports. Personnel and history of the project are also outlined. The investigations cover a wide

range of studies on the ionosphere, especially the lower

ionosphere. These are listed and discussed under the following heads: 1) Low frequency (long wave) studies; 2)

Electromagnetic studies (wave solutions, coupling theory

and total polarization); 3) Ionospheric physics (solar and

high atmospheric physics, D region viscosity, dynamics of

ionized media, effect of vertical ion transport); 4) Ionospheric properties (coupling phenomena, E layer characteristics, ionospheric winds and wave interaction); 5) Applied propagation investigations (oblique incidence studies);

6) Extra terrestrial studies (ring current and electrodynamics

of very high atmosphere); and 7) Long wave equipment development. (Met. Abst. 72. l.)-M.R.

D-359 Kakinuma, Takakiyo, Polarization of solar radio bursts at

microwave frequencies, Pt. 1. Nagoya Univ. Research

Institute of Atmospherics, Proceedings, 5:71-80, March

1958. 6 figs. , 2 tables, 6 refs. DWB--The intensity and

polarization of solar radio bursts have been observed at

9400, 3750, 2000 and 1000 Mc/s since July 1957. In this

paper the results of observations during 6 months are described. In most bursts at microwave frequencies, the difference in the intensity of two circularly polarized components is observed. At 3750 Mc/s, the bursts of small degree of polarization (less than 10%) are predominant, compared with other frequencies. At 200 and 1000 Mc/s the

circularly polarized bursts were occasionally observed, but

not at 9400 and 3750 Mc/s and at 3750 Mc/s the linearly

polarized components were not observed. In most bursts

observed at four frequencies, the sense of polarization re- verses near 3750 or 2000 Mc/s and the degree of polarization is generally small at 3750 Mc/s. At 9400 Mc/s, it

128
seems that the sense of polarization correlates with the

position of the source on the solar disk. Further observations will be continued to investigate the relation between

them. (Met. Abst. 10. 3-202. )--Author's abstract.

D-360 Kakinuma, Takakiyo (Nagoya Univ. ) and Hiei, Eijiro (Tokyo

Astron. Obs.), Unusual decrease of microwave solar radio

emission during flare on Nov. 30. 1959. Astronomical Society of Japan, Tokyo, Publications, 12(1):117-123, 1960. 3

figs. , 2 refs. --Unusual decrease of microwave solar radio

emission on Nov. 30, 1959, observed at the Research Institute of Atmospherics, Nagoya University is reported, together with the optical observations of the associated flare

made at the Tokyo Astronomical Observatory. (Met. Abst.

1 1L -95. )--Authors' abstract.

D-361 Kallmann, H. K. (Calif. Univ. , Los Angeles), The continuous layer formation in the atmosphere under the influence

of solar radiation. Physical Review, 90(1): 153-154, April 1,

1953. 2 figs. , 5 refs. DWB--The continuous increase or decrease of electron density with height under influence of a

quiet and a disturbed sun was investigated. The results,

presented in diagrams, correspond to the order of magnitude

of frequencies as used by the radio technician for E layer re- flections. (Met. Abst. 5. 5-235. )--W. N.

D-362 Kallmann, H. K. , Tentative absorption and emission spectra of the atmosphere. California. Univ. Institute of Geophysics, Contract AF 19(604)-111, Scientific Report, No. 2,

June 30, 1954. 29 p. almost entirely tables, 52 refs. DWB

--Tables of upper atmosphere absorption and emission spectra have been prepared. The absorption spectrum covers a wavelength range from 24 microns to about 300 A. The emission spectra start at 2. 8 and end at 3100 A. The spectra

are arranged in decreasing order of wavelengths. The presentation of these tables is based on an extensive literature

survey made on the subject; 52 references are given. It should be pointed out, however, that the identification of

the element absorbing or emitting a certain wavelength in

several cases is doubtful and might be open to discussion.

Whenever possible, approximate heights, where these absorption or emission in the atmosphere may occur, are indicated. Here again, these heights are only tentative.

Nevertheless, it is hoped that these tables may be useful

to workers in various fields of upper atmospheric research.

(Met. Abst. 7. 1-221. )-Author's abstract.

129
D-363 Kallmann, H. K. ; Kellogg, W. W. ; Rapp, R. R. and Greenfield, S. M. , Scientific use of an artificial satellite. Rand

Corporation, Santa Monica, Calif. , Paper 733, Sept. 6,

1955. 22 p. 26 refs. DWB (M055 R186p)--An early re- view of general areas where there are possible uses for

earth satellites in studies of solar radiation, in the UV and

X-ray region, electron density measurements; pressure, density and atmospheric composition measurements; cosmic

rays, albedo of the earth, artificial seeding of the atmosphere, geodetic measurement, and cosmic or solar high frequency radio noise. (Met. Abst. 11J-83. )--M. R.

D-364 Kamiya, Yoshiko (Physical Inst. , Nagoya Univ. ) and

Wada, Masami (Inst, of Physical and Chemical Research),

Cosmic ray storms and solar radio outbursts. Japan. Science Council. Ionosphere Research Committee, Report of

Ionosphere and Space Research in Japan, 13(2): 105-111,

1959. 4 figs. , 2 tables, 9 refs. DLC -Relations between

the type of solar radio outburst, cosmic ray storm and magnetic storm are studied using the data obtained during IGY,

and the following results are obtained. 1. Almost all cosmic ray storms are associated with Type IV solar radio outbursts. 2. The other types of outbursts are not related to

cosmic ray storms. 3. The size of a cosmic ray storm is

independent of the meridian distance of the radio outburst,

but that of a magnetic storm depends on it. From these re- sults, it can be concluded that a large corpuscular cloud

with magnetic field is emitted simultaneously with Type IV

solar radio outburst occurrence and it has a small core which

is the cause of the magnetic storm. (Met. Abst. 11. 8-89.

)

--Authors' abstract.

D-365 Kamiyama, Hiroshi (Tohoku Univ. ), Variation of the effectiveness of the solar flare according to its location. Tohoku

University, Science Reports, 5th Ser. , Geophysics, 4(1):

1-4, June 1952. 3 figs. , 2 tables, 5 refs. MH-BH-A statistical method is adopted for investigation of the longitudinal effect of a solar eruption upon radio communication.

Six hundred and forty eruptions were observed and analyzed

during the past four years. The most pronounced effect was

found at 30HE — 10 W decreasing to a half beyond both 50

meridians. Results are presented in curves and tables.

(Met. Abst. 5. 3-308. )-W. N.

D-366 Karpov, A. N. , Izmenenie sily radios iqnalov vo vremia

solnechnoqo zatmeniia 30 iiunia 1954 qoda. (Change of

radio signal intensity during the solar eclipse of June 30,

1954.) Priroda, Moscow, 44(5):113, May 1955. fig. DLC--

Reception of short wave radio signals during solar eclipses

when radiation flow is shut off by the moon is one of the

130
methods of studying the ionized oxygen layer. Such a study was carried out on the morning of June 30, 1954, at

the Stalingrad Medical Institute during reception of radio

signals from the Moscow radio station with about 25 m

wave length. The received signals were compared with

signals of a 2 scale sound generator enabling to change

smoothly the frequency and level of the signals within one

decibel. It has been established that during the eclipse

the intensity of the signals decreased by 48 decibels, and

dropped almost to zero at the midpoint of the eclipse. An

attached graph shows that the attenuation curve of the

radio signal reception coincides almost completely with

the phases of the eclipse. This denotes the comparatively

large speed of recombination of ionized particles in the atmosphere in the absence of solar radiation, and the great

sensitivity of the layer to all changes of solar activity.

(Met. Abst. 9A-78. )--A. M.P.

D-367 Kato, Yoshio; Kamiyama, H. and Kikuchi, Takehiko,

Report on the result of the observation of the signal strength

during the partial solar eclipse of Sept. 12, 1950. Sendai,

Japan. Tohoku Univ. , Science Report, 5th Ser. Geophysics,

3(2):53-56, Sept. 1951. 3 figs. , 2 tables. DWB-Measurements of the signal strength of radio waves were made during

the half month in which the partial solar eclipse occurred in

order to study the behavior of the lower ionosphere. (Met.

Abst. 6D-75.)--A.A.

D-368 Kato, Yoshio and Watanabe, Tomiya (both, Geophysical

Inst. , Tohoku Univ. , Sendai), Studies on P. S.C. (Polar

sudden commencements) . Japan. Science Council. Ionosphere Research Committee, Report on Ionosphere Research

in Japan, 10(2):69-80, 1956. 6 figs. , 2 tables, 18refs.,

10 eqs. DWB--Facts obtained from observations of p. s.c. suggest that its origin is outside the ionosphere. Particularly, the daily behavior of the horizontal perturbing vector

of p. s. c. can be explained by the shielding effect of the

non -uniform ionosphere. (Met. Abst. 11F-64. )- -Authors'

abstract.

D-369 Kazantsev, A. N. (Academy of Sciences of the U.S.S. R. ),

Absorption and electron distribution in the F2 layer determined from measurements of transmitted radio signals from

earth satellites. Planetary and Space Science, N. Y. , 1(2):

130-135, April 1959. 6 figs., 3 refs. , 7 eqs. DWB--Comparison is made between measured field strengths of transmitted signals from earth satellites and those theoretically

predicted when the transmitter position is in the region of

maximum electron concentration of the F2 layer, below it,

and above it. The observed absorption value agrees best

131
for a biparabolic distribution with exponential continuation

-3

with K = 8 X 10 where the electron concentration is given

-kh by N - N e . The number of electrons per column in the

13

upper region of the F2 layer is deduced to be 1. 5 X 10

2

electrons per cm . This value is compared to the findings

of BURGESS. Curves are given of field strengths at distances greater than 10, 000 km. At distances of 16, 000 km

the formation of ionospheric wave guides makes possible

the transmission of radio signals. (Met. Abst. 11E-74. )--

Author's abstract.

D-370 Kazes, Ilya and Steinberg, J. L. , Etude du rayonnement

radioelectricrue solaire sur 9350 MHz au voisinaqe du

coucher et du lever soleil. (Study of radio electric solar

radiation at 9350 MHz at the vicinity of sunset and sunrise.

)

Academie des Sciences, Paris, Comptes Rendus, 240(5):

493-495, Jan. 31, 1955. 2 figs. DLC--A study of atmospheric absorption and refraction. CSIRO Abstract.

D-371 Kazes, I. , Etude de la scintillation du soleil observee sur

la longueur d'onde de 3. 2 cm. (Study on solar scintillation

observed on 3. 2 cm wavelength. ) Academie des Sciences,

Paris, Comptes Rendus, 245(6): 636-639, Aug. 5, 1957. 2

figs., 3 refs. Also: Kazes, I. and Steinberg, Jean-Louis,

Etude de la scintillation du soleil observee avec plusieurs

antennes sur la longueur d'onde de 3. 2 cm. (Study of solar

scintillation observed with several antennas on 3. 2 cm wavelength. ) Ibid., 245(7): 782-785, Aug. 12, 1957. 3 figs. , 2

refs. DWB--Fluctuations in solar radiation at 3.2 cm wavelength are shown to be of atmospheric origin. Effects of

solar activity, wavelength and zenith distance on these fluctuations are discussed. According to the second paper the

fluctuations were identified as shadow zones whose movements showed qualitative agreement with winds at the height

of the tropopause. (Met. Abst. 9A-171. )--G.T.

D-372 Kazes, I. and Steinberg, J. L. , Etude de la scintillation du

soleil observee avec plusieurs antennes sur la longueur

d'onde de 3. 2 cm. (Study of the sun's scintillation observed

by means of several antennae on 3. 2 cm wavelength.

)

Academie des Sciences, Paris, Comptes Rendus, 245(7):782-

785, Aug. 12, 1957. 3 figs. , 2 refs. DLC -Scintillation

measurements made with three receivers located at variable

distances allowed to state precisely the average size (170m)

of cast shadows on the soil and to compare their speed with

the wind velocity at tropopause altitude. In spite of the distance between stations, and the differences of several hours

existing between meteorological and radioelectrical observa132
tions, winds of same directions are always observed. Scintillations are very likely produced in the low atmosphere at

an altitude close to the irregularities responsible for optic

scintillations. (Met. Abst. 10. 1-344. )--A. V.

D-373 Kell, R.E. (Cornell Aeronautical Lab. ), The effect of Dop- pler broadening upon radar cross section of a plasma sur- rounded body. Planetary and Space Science, N. Y. , 6:225# June 1961. Abstract only. The paper was presented at the

Plasma Sheat Symposium, Boston, Mass. , Dec. 7-9, 1959.

--The radar signal scattered from a plasma may be considered as the vector sum of the signals scattered from the individual electrons of the plasma. If the electrons have a component of motion radial with respect to the radar, the

signal from each electron will possess a Doppler shift in

accordance with its radial velocity, and an originally monochromatic illuminating electromagnetic wave will be scattered as a non-monochromatic spectrum of waves, where the

spectral distribution represents the distribution of radial

velocity for the electrons. The effects of Doppler spectral

broadening upon radar cross section will be discussed, and

experiments to determine the magnitude and shape of the

broadened spectrum will be described.

D-374 Kellogg, William W. (Rand Corp. , Santa Monica, Calif. ), IGY rockets and satellites: a report on the Moscow meetings , Aug. 1958. Planetary and Space Science, N. Y. , London,

l(l):71-84, Jan. 1959. 5 refs. DLC--This report summarizes

the proceedings of the Technical Symposia on Rockets and

Satellites. Tremendous strides have been made in the ex- ploration of the upper atmosphere and the space beyond by

new vehicles. In the summary/ the subject matter rather

than the vehicle is the central theme. The summary includes

chapters on: 1) atmospheric structure; 2) electromagnetic

properties of the ionosphere; 3) cosmic and auroral particles; 4) solar and stellar ultraviolet and X-ray radiation;

5) micrometeorites; 6) biological experiments; 7) rocket

and satellite instrumentation and special applications; 8)

reviews of rocket programs; and 9) satellite programs. (Met.

Abst. 111-131. )--E.K.

D-375 Kellogg, W. W. , Review of IGY upper air results. Rand

Corp. , Santa Monica, Calif. , Paper 1717, June 5, 1959.

21 p. 5 figs. , numerous refs. DLC --Recent findings concerning conditions in the stratosphere, mesosphere, and

ionosphere are discussed in that order. In the lower stratosphere, improved balloon soundings have made it possible to

draw constant pressure charts up to the 10 mb level. Rapid

wanning processes and the use of ozone and radioactive

debris as tracers are briefly discussed. For the higher

133
atmosphere, density and pressure values obtained from rockets and satellites and compiled by KALLMANN (Rand Paper

1591, Jan. 1959) are reproduced to illustrate mean conditions. Diurnal variations in density revealed by NRL rocket

observations at Ft. Churchill, and recent data on atmospheric

composition from the Univ. of Michigan and NRL are discussed. In the final section, solar terrestrial relationships

are taken up, with special mention of the close correlation

of 10 to 20 cm radio emanations from the sun with satellite

observed densities. (Met. Abst. 111-160. )--R. S.Quiroz.

D-376 Kelly, Joseph J. (Martin Co. , Md. ), Earth satellites.

Weatherwise, Boston, 8(5): 121-122, Oct. 1955. photo.

DWB--The value of an earth satellite to meteorology is discussed. Suggested measurements include analysis of specific infrared band from earth, "strength and direction of the

high frequency radio communications link as it sweeps

through the atmosphere/' measurement of solar radiation

outside the atmosphere, influence of meteoric dust upon

the attenuation of radiation. (Met. Abst. 8. 6-63. )--I.L.D.

D-377 Kelso, John M. , Doppler shifts and Faraday rotation of

radio signals in a time varying, inhomogeneous ionosphere.

Pt. 1: Single signal case. Journal of Geophysical Research,

65(12): 3909-3914, Dec. 1960. fig., 8 refs. , 24 eqs. Also:

Pt. 2: Two signal case. Ibid., 66(4):1107-1115, April 1961.

DLC --Equations are derived for the frequency shift of a radio

signal transmitted to the ground from a space vehicle in or above the ionosphere. The principal restriction on the generality of the results is that the ionosphere is treated as

quasi-isotropic; i. e. the ray paths are obtained by methods

which would be exact in a slowly varying isotropic medium,

but the refractive index is permitted to be a function of ray

direction (implying an anisotropic ionosphere). The following conditions prevail: (a) the (slowly varying) ionosphere

may be a general function of three spatial coordinates of

time; (b) the vehicle may follow an arbitrary (nonrelavistic)

trajectory; (c) the magnetic field, which characterizes the

dependence of the refractive index on direction, may have

arbitrary form. The same conditions as for Pt. 1 are used

in Pt. 2. Equations are obtained for the time rate of change

of the phase difference between two signals whose refractive indices are slightly different. The results are applied

to the frequency shifts experienced in a two frequency Doppler experiment of the Seddon-Jacks on type, and to the determination of the rate of Faraday rotation of the plane of

polarization. --Author's abstract.

134
D-378 Kent, G.S. (Cavendish Lab. , Cambridge), High frequency

fading observed on the 40 Mc/s wave radiated from artificial

satellite 1957 06. Journal of Atmospheric and Terrestrial

Physics, N.Y. , 16(1/2): 10-20, Oct. 1959. 8 figs. , 9refs.,

eq. DWB, DLC--A study has been made of high frequency

fading observed on the 40 Mc/s wave radiated from the first

Russian satellite (1957 00 ). This fading had a frequency

of a few cycles per second and it is concluded that it was

produced by the passage of the waves through irregularities

in the F region of the ionosphere. The size and spatial distribution of these irregularities have been examined, and it

is found that they are about 1 km in size and that they occur

at heights above about 250 km. They usually occur at latitudes greater than 50 N and are more concentrated toward

the north. It is likely that their density is controlled by

magnetic rather than geographic latitude and there is a tendency for them to be grouped into large areas. These have

dimensions of several hundred kilometers and are elongated

along the parallels of latitude. Comparison is made of the

properties of these irregularities with those believed to be

responsible for radio-stellar scintillation and spread F echoes. (Met. Abst. 11E-75.)- -Author's abstract.

D-379 Kerr, F.J. and Shain, C.A. , Moon echoes and transmission

through the ionosphere. Institute of Radio Engineers, Proceedings, 39(3): 230-242, March 1951. 12 figs. , table, 29

refs. , 16 eqs. DLC--Over a year's time, thirty experiments

of moon echoes of about 20 Mc frequency were carried out,

and these conclusions were drawn: (1) echo intensities

lower than expected; (2) minimum altitude of echo higher

than expected; (3) anomalous values of echo intensities and

minimum detection altitude correlate with foF2; (4) slow fading was consistent with ionospheric origin; (5) fast fading

was associated with the moon's libration; (6) millisecond

pulses were elongated on reflection from moon, and (7) ray

deviations of several degrees in vertical plane apparently

occurred. (This paper is of interest to meteorologists because of its negative aspects.) (Met. Abst. 2H-212.

)

D-380 Kerr, Frank J. ; Shain, C.A. and Kraus, John D. , Reflexion of radio waves from the moon. Nature, London, 179

(4556):433, Feb. 23, 1957. 2 refs. DWB-KERR and

SHAIN found reflection of 14 m waves from moon of level

to be expected from a nonabs orbing isotropic moon; there

is no evidence of the specular reflection postulated by

KRAUS. KRAUS suggests that reflection was from a cloud

of charged particles temporarily associated with the moon.

(Met. Abst. 10. 2-lll.)-C.E.P.B.

135
D-381 Kerr, F. J. , Radio echoes from sun, moon and planets.

Handbuch der Physik, Berlin, 52:449-464, 1959. 8 figs.

,

table, numerous refs. , 11 eqs. DWB-- A review of knowledge up to 1958 of radar echoes and their characteristics,

or possible characteristics, when reflected from the moon

(since 1946), the sun and the planets (if and when accomplished), and from the ionosphere aurora, meteors, whistlers, etc. Future possibilities are as challenging as the

actual performance is remarkable. Radio communications

via the moon are discussed in some detail and references

cited systematically. (Met. Abst. 11H-73. )--M. R.

D-382 Khaikin, S.E. , Radioastronomiia i izuchenie vselennoi.

(Radioastronomy and the study of the universe. ) Priroda,

45(8):5-14, 1956. 6 figs. (incl. photos). DLC--The author

discusses the radio wave radiation of various cosmic bodies both heat radio wave radiation, non-heat radio wave

radiation and the theories accounting for radio waves of

non-heat origin, the conditions for the propagation of radio

waves and the characteristics of radio telescopes; including their sensitivity and resolving power. (Met. Abst. 9A163.)»I.L.D.

D-383 Kiepenheuer, Karl, The sun. Ann Arbor, Michigan, Univ.

of Michigan Press, 1959. 160 p. 76 figs. (incl. photos).

DLC (QB521.K613). Transl. by A. J. Pomerans of the original German, Die Sonne, issued Berlin, Springer-Verlag,

1957. 150 p. figs. (Verstandliche Wissenschaft, Vol. 68)

DLC (QB521. K6). Review by Ralph Shapiro in American

Meteorological Society, Bulletin, 41(5):281-282, May 1960.

--A well illustrated and not-too-technical text on the nature

of the sun as the only star we can observe in detail, and

its relation to terrestrial phenomena. Solar physics, solar

research, the solar system (planets, comets, meteors, zo- diacal lights, dust and gas); the sun's surface (granulation); solar radiation (use, solar constant, solar temperature, spectrum, spectroscope, chemical composition of sun);

solar spectrographs and telescopes; eclipses; sunspots and

solar changes (magnetic fields, faculae, flares, filaments,

storms, prominences, corona); the interior of the sun; radio

waves and bursts and, finally, solar terrestrial and weather

relations. (Met. Abst. 11. 2-15. )-M. R.

D-384 Kimpara, Atsushi (Nagoya Univ. ), S.I. D. phenomena on

Nov. 22, 1952. Japan. Science Council. Ionosphere Research Committee, Report of Ionosphere in Japan, 7(4): 158,

Dec. 1953. DWB--Brief note reporting S. I. D. phenomenon

at time of low solar activity, revealing close correlation of

solar flares with outburst of solar radio waves. Atmospherics

were found to increase an hour before the solar flare. (Met.

Abst. 6. 8-159. )--G.T.

136
D-385 Kimpara, A. , The sudden ionospheric disturbances on Nov.

22. 1952. Nagoya. Univ. Research Institute of Atmospherics, Proceedings, 2:40-52, Jan. 1954. 11 figs. , 5

tables. Append, p. 48. DWB--Despite the period of lower

solar activity, a striking S. I. D. phenomenon was observed

on Nov. 22, 1952, which revealed the close correlation of

solar flare with outbursts of solar radio waves, Dellinger

fadeout in short wave communication, characteristic crochets in three components of magnetograms, fadeout of echoes

in ionospheric measurements, and an abnormal increase of

the intensity of atmospherics at very low frequencies. The

author made a detailed study of these relations and found

an advance increase of the intensity of atmospherics about

an hour before the solar flare. He appends similar results

obtained in a more active period (April, May 1952) as a reference, and discusses their characteristics and correlations,

(Met. Abst. 6D-249. )- -Author's abstract.

D-386 King, G. A. M. (Geophysical Obs. , Christchurch, New

Zealand), The ionospheric E layer at Cape Hallett. Journal

of Atmospheric and Terrestrial Physics, London, 16(1/2):

18S-187, Oct. 1959. table. DWB, DLC -Ionograms from

April 20 - Aug. 14, 1958 for studying the variations with

solar zenith angle of foE using 1-2 Mc/s frequency facilitating separation of UV ionization and that from particle

influx are compared against values expected from a model

ionosphere. The calculated values of foE are in good agreement with the observed ones. (Met. Abst. 11. 12-381.)--

W.N.

D-387 Kisliakov, A. G. , Rezul'taty eksperimentarnoqo issledovaniia radioizlucheniia Luny v chetyrekhmillimetrovom

diapazone voln. (Results of an experimental study of radio

emission of the Moon in the four millimeter diapason.

Astronomicheskii Zhurnal, Moscow, 38(3):561-563, May/

June 1961. 7 figs. , 9 refs. , 3 eqs. Russian and English

summaries p. 561-562. DLC. Transl. into English in the

corresponding issue of Soviet Astronomy AJ, N. Y. --Data of

the radio emission of the Moon in the four millimeter diapason, obtained during the summer of 1960 by the "Elbrus*

expedition of the Radio Physical Institute, are given. It is

found that the phase variations of radiation intensity of the

Moon can be approximated satisfactorily by the relation

T n = 230 + 73 cos ( jr t-24°) °K. The derived results

agree with the theory developed for a unilayer model of the

lunar surface. (Met. Abst. unpub. ) --Author's abstract.

137
D-388 Kirshnamurthi, M. ; Sivarama Sastry, G. and Seshagiri

Rao, T. (all. Physical Lab. Osmania Univ. , Hyderabad),

Radio emission from the sun at 30 Mc/s . Journal of Scientific and Industrial Research, Sec. A, New Delhi, 17(12),

Special Supplement, Dec. 1958. p. 71-73. table, 5 refs.

DWB, DLC--The observations tabulated and discussed were

conducted from May 1 to Aug. 31, 1958 by instrumentation

described in detail. No radiation from the direct sun was

observed, indicating its temperature at this frequency <

52, 000 K since the minimum detectable difference between source and background is calculated to be 40, 000 K.

Enhanced radiation was observed 40 times, of which only

four could be associated with flares. (Met. Abst. 11.6-

146.)--W.N.

D-389 Kitchen, F. A. and Joy, *W. R. R. (both, Royal Naval Scientific Service), Some effects of the fine structure of the ionosphere on transmissions received from the Russian earth

satellite 1958 8 . Nature, London, 181(4626): 1759-1761,

June 28, 1958. 3 figs. , table, 7 refs. D"WB--After some

simultaneous direction finding and Doppler frequency shift

measurements had been made on the radio transmissions

from the Russian satellite 1958 £ , on a frequency of

20. 005 Mc/s with the initial object of obtaining the parameters of local tracks and those of the orbit, the authors

set up a table for Portsdown, England, during the period

May 16-22, 1958. Interesting anomalies observed then

are listed. (Met. Abst. 10. 8-95. )--N. N.

D-390 Klee, Ernst (Munich), Satellitenprogramm der Volkssternwarte Munchen. (Satellite program of the National Astronomical Observatory at Munich. ) Naturwissenschaftliche

Rundschau, Stuttgart, 11(1) :7-8, Jan. 1958. fig. DWB,

DLC--In order to record the continuing line emitted by Sputnik at a frequency of 40. 002 MHz after it had ceased to

broadcast at 20. 005 MHz, the National Astronomical Observatory obtained a new receiver which includes the re- gion 30-180 MHz with an entrance sensitivity of 0. 1 y&V.

With this receiver 36 curves were obtained during the period

Oct. 10-Oct. 24, 1957. The diagram (reproduced in this

paper) shows a satellite passage on Oct. 13th. The curves

show a distinct maximum at 22 hrs 13 min 47 sec, that is,

17 sec after passing over Paris. A marked impulse peak is

apparent at 22 hrs 16 min 45 sec as the satellite enters the

U. S.S. R. The intensity of this signal which attains 2/3 of

its maximum at a distance of about 1000 km may indicate

that a measurement signal is emitted either from the satellite or from a ground station at the same frequency. (Met.

Abst. 11. 1-111. )-I.L.D.

138
D-391 Klein, M. M. ; Greyber, H. D. ; King, J.I.F. (all, Missile

and Space Vehicle Dept. , Gen. Elec. Co. , Phila. ) et al.

,

Interaction of a non-uniform plasma with microwave radiation. Planetary and Space Science, N. Y. , 6:105-115, June

1961. 7 figs. , 7 refs. , 50 eqs. DWB--The topic is discussed in terms of normal and non-normal incidence of radiation. The latter case in the short wavelength region only.

Absorption coefficient varies insignificantly, remains large

over range of angles of incidence, dropping off rapidly beyond 45 . --W. N.

D-392 Klinger, Hans Herbert, Solare und kosmische Radiowellen.

(Solar and cosmic radio waves.) Experientia, Basel, 8(9):

325-336, Sept. 15, 1952. 14 figs., 3 tables, refs., eqs.

English summary p. 336. DWB--After discussing the physics of black body radiation and its reception, author describes and illustrates solar radio radiation of 3 types —

constant thermic radiation from the spot-free sun, sunspot

radiation and eruptive radiation. Cosmic radio waves are also discussed and analyzed. (Met. Abst. 4.9-105.)--

C. E. P. B.

D-393 Knuth, Robert; Klinker, Ludwig; Schmelovsky, Karl Heinz

(all, Obs. fur Ionospharenforschung, K&hlungsborn) et al.

,

Die Elektronenkonzentration in der ausseren Ionosphare:

Messungen des Sommers 1959. (The electron concentration

in the outer ionosphere: measurements in the summer of

1959.) Beitrage zur Geophysik, Leipzig, 70(4):201-212,

1961. 6 figs., table, 10 refs. , eqs. German and English

summaries p. 201. DWB, DLC—From Faraday fading measurements during summer 1959 the formerly received results

are generally confirmed. The diurnal variation of electron

content deduced from two-hourly means has a slight but distinct minimum just after noon. The observed decrease in

electron content since summer 1958 is not significant. The

plasma scale heights for summers 1958 and 1959, calculated by different methods, agree in a sufficient manner. The

total electron number decreases toward south (mean value

0.6%/ 100 km). This gradient shows diurnal variations with

the maximum at noon. Former investigations about statistical relations between the irregular variations of electron

content and those of foF2 are continued. For the disturbed

periods of July and Aug. 1959 marked pre-storm increases

are found as formerly reported. (Met. Abst. unpub. )--

Authors' abstract.

139
D-394 Ko, H. C. f The distribution of cosmic radio background • radiation. Institute of Radio Engineers, N. Y. , Proceedings, 46(1): 208-215, Jan. 1958. 12 figs. , table, 34 refs.

DLC--The results of a survey of cosmic radio background

radiation at 250 Mc, using the Ohio State University 96 - helix radio telescope, are described. Eight maps for frequencies from 64 Mc to 910 Mc are presented. Radio maps

made at other frequencies by various groups are summarized.

Comparisons of the maps showed consistent features represented by three symmetrical distributions and several irregular ones discussed. (Met. Abst. unpub. )- -From Author's

abstract.

D-395 Ko, H. C. (Radio Obs. , Dept. of Elec. Eng. , Ohio St.

Univ. ), Amplitude scintillation of extraterrestrial radio

waves at ultra high frequency. Institute of Radio Engineers,

N.Y. , Proceedings, 46(11):1872, Nov. 1958. 3 figs. DWB

—Radio stars exhibit fluctuations because of the irregularities in the earth's ionosphere. These irregularities have

different radio frequency refractive indexes and thus present

some important effects on the propagation of radio waves.

Scintillation measurements made from Ohio State University

Radio Observatory (lat. 40°01' N; long. 83°03" W) are re- ported. This is a preliminary report on research that is continuing. (Met. Abst. 11. 7-166. )--N.N.

D-396 Ko, H. C. , Amplitude scintillation of radio star at ultrahigh frequency. Institute of Radio Engineers, N. Y. , Proceedings, 48(11): 1871 -1880, Nov. 1960. 13 figs. , 22 refs.

,

eq. DWB--Experimental results of the Cygnus A observations at 915 Mc, as conducted at the Ohio State Univ. Radio

Observatory, Oct. 1957-Sept. 1958, are presented graphically and discussed. The observational equipment described

included at 400 ft diameter parabolic antenna rotationally

tracking Cygnus A from rising to setting. The radio meter

was a UHF total power low noise type. The fluctuation rate

of scintillation was about 1/2 to 8 peaks per minute and

averaged about 15% near horizon. Scintillation decreased

rapidly with increased elevation angle, showed marked seasonal but insignificant diurnal variation. K index correlation with fluctuation rate at 915 Mc existed in winter months

only. Marked effects of auroras and geomagnetic disturbances indicate mainly ionospheric and, but partially, tropospheric origin of scintillation at 915 Mc. --W. N.

D-397 Koeckelenbergh, A. , L' eruption chromospherique du 9 avril

1956 et ses phenomenes associes. (The chromospheric eruption of April 9, 1956, and its associated phenomena.) Ciel

et Terre, Brussels, 75(1/2): 28-33, Jan. /Feb. 1959. 2 figs.

,

2 pi. , 6 refs. DLC--

140
On April 9, 1956, a particularly intense chromospheric

eruption was observed at the Royal Observatory of Belgium.

A solar radio jump on 169 MHz was recorded at the same

time, at the radio astronomical station at Humain-Rochefort

(Belgium) and a practically general disturbance was noted

on short waves. The author gives the observation conditions, the optical data and the radioelectric observations

made on 169 MHz as concerns this phenomenon. He examines the ionospheric effects and the geomagnetic effects

and compares the data gathered. The ionospheric disturbance was preceded by optical, geomagnetic and radioelectric phenomena on meter waves. It began at the moment of

the maximum emission on the H line. It probably is connected with a simultaneous reinforcement of this line and

of the ultraviolet L line or the solar X radiation. (Met.

Abst. 11D-73.)--

D-398 Koeckelenbergh, A. , Evolution d'un filament sombre lors

de l'eruption solaire du 16 Juillet 1959 (16 h 08 m TU) . (Evolution of a dark surge at the time of the solar eruption

on July 16, 1959 (16 h 08 m UT). ) Ciel et Terre, Brussels,

76(7/8): 216-220, July/Aug. 1960. fig., 3 plates, 8 refs.

DWB, DLC- -Description of the eruption of July 16, 1959,

which occurred in a zone of heliographic coordinates 14 N

22 W. At the same time an important dark surge developed

which showed a considerable asymmetry of the H Celine profile. There is reason to believe that it was an arch shaped

prominence. The author gives a summary of the phenomena

associated with this eruption. The conditions of ionospheric propagation were highly disturbed from July 15, and a magnetic disturbance was observed on July 17 at the geomagnetic station of Manhay (Belgium). Again a marked agreement was observed between the sudden enhancement of

sferics and the optical eruptions. (Met. Abst. 11L-283. )--

A.V.

D-399 Komesaroff, M. M. (Div. of Radiophysics, C.S. I. R.O.

Univ. Grounds, Chippendale, N. S. W. ), Polarization measurements of the three spectral types of solar radio burst.

Australian Journal of Physics, Melbourne, 11(2):201-214,

June 1958. 6 figs. , 2 tables, 8 refs. , eqs. DLC--A sweptfrequency technique was used for measuring the polarization

of solar radio bursts occurring at the beginning of the present sunspot cycle. Of special interest were the results for

barsts of spectral type III. Contrary to the inference drawn

from earlier work, it was found that many of these bursts

are highly polarized. Furthermore, there were strong indications that the polarization is produced at the radiation

source and is not imposed by propagation conditions in the

overlying media. (Met. Abst. 10. 2-224. )- -Author's abstract

141
D-400 Komesaroff, M.M. and Shain, C.A. , Refraction of extraterrestrial radio waves in the ionosphere. Nature, London,

183(4675): 1584-1585, June 6, 1959. fig., 5 refs. , 3 eqs*

DLC--New expressions derived for refraction, taking into

account the effects of horizontal gradients in electron density and considering the magnitude of the uncertainties involved in the necessary approximations are demonstrated.

The analysis is restricted to the case of a transit radio telescope. The astronomical value of the ionospheric refraction

corrections, the observed and corrected positions are indicated graphically. (Met. Abst. 1IE -81. ) —From authors'

text.

D-401 Korowski, E. T. (General Electric Co. ), The region behind

a body moving through a rarefied ionized atmosphere. Planetary and Space Science, N. Y. , 6:223-224, June 1961. Abstract only. The paper was presented at the Plasma Sheath

Symposium, Boston, Mass. , Dec. 7-9, 1959. --Physical

arguments indicate that charge density gradients will exist

some distance behind and possibly a short distance to the

side of a body moving at high speed through the ionized

layers of the upper atmosphere. The medium is taken to be

highly rarefied gas composed of ions and electrons. An un- steady model is set up, wherein the ion and electron density profiles, which are obtained as a function of space and

time, correspond to the profiles at a given cross section aft

of the body in the actual problem. The Boltzmann equation

with electric effects taken into account is utilized and solutions are obtained numerically. Perturbations on the velocity distribution functions are calculated over small increments of time which then yield the magnitude of the electric

effect over the next time increment. Calculations indicate

that the charge density gradients extend several body radii

downstream. These gradients are inherent to the rarefied

flow over any vehicle and can significantly alter its detectability by electromagnetic signals.

D-402 Koster, J. R. (Univ. College of Ghana, W.Africa), Radio

star scintillations at an eguatorial station. Journal of Atmospheric and Terrestrial Physics, London, 12(2/3): 100-109,

1958. 4 figs. , 4 tables, 10 refs. DLC -Radio star scintillations have been observed at a frequency of 45 Mc/s over

a period of 4 yrs at an equatorial station with a phase switching interferometer. Scintillation effects are found to be very

severe, the output from even intense radio stars often dropping to zero. Scintillation occurs only at night, and is of

nearly daily occurrence near sunspot maximum, correlating

positively with the sunspot cycle. It correlates highly with

the occurrence of spread F echoes, but with no other geophysical phenomena. It is as yet unclear whether the

142
observed results are due to absorption of the signal or can

be accounted for by the impression of a much larger phase

deviation on the emergent wave front by the diffracting

screen responsible fpr scintillation. The phenomenon cor- relates highly with the trans equatorial scatter of radio signals observed near sunspot maximum. (Met. Abst. 10. 2-

331. )--Author's abstract.

D-403 Krasovskii, V.I. , Sovetskie issledovaniia ionosfery pri

pomoshchi raket i iskusstvennykh sputnikov Zemli. (Soviet

exploration of the ionosphere by rockets and artificial earth

satellites.) Iskusstvennye Sputniki Zemli, Moscow, No.

2:36-49, 1958. 15 figs. , 16refs., 4 eqs. DLC. Transl.

into English issued in Artificial Earth Satellites, issued

N. Y. , Plenum Press; London, Chapman & Hall, 1960. Vol.

2:45-62. --A review of the principal studies in the ionosphere

by means of rockets and artificial earth satellites carried out

in the U.S.S. R. The methods for making these studies involved the use of the disperse interferometer which measured

the radio waves radiated from the rocket and the satellite,

the direct measurement of the concentration of charged particles in the ionosphere, and the transmission of the reading

by telemetric systems. The apparatus are described with

the aid of diagrams and photographs and the results of individual rocket and satellite ascents are presented in graphs.

The ionization above the maximum of the F2 layer declines

very slowly with height so that the altitude scale for ionizing particles is very large; at 475 km an ionization of about

1CP electrons mets/cm3 was recorded on Feb. 21, 1958; at

795 km the concentration of positive ions reached 1. 9 X 10^

ion/cm^ on May 15, 1958. The effective temperature of electrons in the F region and above was higher than the temperature of the environment. The ionosphere below the maximum

of the F region, in contrast to its model, constructed on the

basis of ionospheric probing from the earth, does not have

sharply demarcated layers but is characterized by a small

maxima with monatomic increase in electron density up to

the maximum of the F2 layer. The maximum of the F2 layer,

and in general the ionization below this region, is 50-150 km

below the values of the usual ionospheric probing from the

earth. The equations for computing the mean electron density at a given elevation, the current of the collector in the

direct determination of ion concentration, and the deceleration potential are presented in appendices. (Met. Abst.

HF-70.)-I.L.D.

143
D-404 Krasovskii, V. I. ; Kushner, Iu. M. ; Bordovskii, G. A. ; Zakharov, G. F. and Svetlitskii, E. M. , The observation of

corpuscles by means of the third artificial satellite. Planetary and Space Science, N. Y. , 5(3):248-249, July 1961.

Transl. by R. Matthews of original Russian in Iskusstvennye Sputniki Zemli, Moscow, No. 2:59, 1958. ref. DLC--

Two corpuscular stream indicators in the third Soviet satellite gave intense signals May 15, 1958. Although too early

to make any conclusive statement, the observation may perhaps be explained as upper air electron acceleration as a re- sult of the varying magnetic fields in the solar corpuscular

stream. Day time increase in electron fluxes is explained

tentatively too. --W. N.

D-405 Kraus, John D. and Ko, H. C. , A detailed radio map of the • sky. Nature, London, 175(4447): 159-161, Jan. 22, 1955.

2 figs. , 5 refs. DWB--A mercator map of radio brightness

of the sky on 250 Mc/s at Ohio is given. The galactic nucleus stands out as a sharp peak, profiles through which are shown. (Met, Abst. 9A-79. )--C. E. P. B.

D-406 Kraus, J. D. , Distribution of radio brightness across the

Andromeda nebula . Nature, London, 175(4455): 502-503,

March 19, 1955. 2 figs. , 5 refs. DWB--Discussion with

average profiles of radio brightness compared with optical

brightness. The latter shows a smaller area for the nebula.

(Met. Abst. 9A-80. )--C.E.P.B.

D-407 Kraus, J. D. ; Ko, H. C. and Stoutenburg, D.V., A fluctuating celestial radio source at 240 megacycles per second. Nature, London, 176(4476): 304-305, Aug. 13, 1955. fig. , 2

refs. DWB--A radio source near the antigalactic center increased by a factor of 6 in fluctuations with a period of 2-3

min. The fluctuations are believed to be intrinsic. (Met.

Abst. 9A-81.)-C.E.P.B.

D-408 Kraus, J. D. (Radio Obs. , Ohio State Univ. ), Planetary and

solar radio emission at 11 meters wavelength. Institute of

Radio Engineers, N. Y. , Proceedings, 46(l):26o-274, Jan.

1958. 12 figs. , 16 refs. DLC- -Observations are described

of radio emissions from the Sun, Jupiter, and Venus, during

1956 and early 1957 at a wavelength of 11 m. Records are presented of solar 11 meter radiation at the time of a large

(importance 3) flare on Aug. 31, 1956, and during other periods of solar activity. The effect of scintillation on records

of radio stars also is illustrated. A number of records of impulsive radiation from Jupiter at both slow and fast recorder

speeds is shown. Many of the short pulses consist of distinct pairs or triplets. An echo mechanism to explain the

multiple pulses is postulated and observed trends in pulse

144
separation compared to those expected with such a mechanism. The stronger Jupiter pulses indicate a peak radiated

radio power at the source of the order of 10 kilowatts per

cps bandwidth. Observations of 11 m radio emission from

Venus are described and one record is presented for which

the probability is only about one in a hundred thousand that

it is due to a random process instead of Venusian radiation.

(Met. Abst. 11. 5-158. )--Author's abstract.

D-409 Kraus, J. D. and Drees e, E.E. , Sputnik I's last days in

orbit . Institute of Radio Engineers, Proceedings, 46(9):

1580-1587, Sept. 1958. 7 figs., foot-refs. , 2 eqs. DLC--

Observations during the last days of Sputnik I's orbiting are presented. These observations were made at the Ohio State

Univ. Radio Observatory, using a simple CW reflection

technique. The data suggest that the breakup of an artificial satellite upon its re-entry into the denser atmosphere

ia a complex phenomenon in which a sequential series of

events may occur over a period of days. Graphs of the aver- age height of the satellite and its associated fragments as a function of time are presented, and some conclusions are drawn as to the details of the actual breakup phenomenon.

(Met. Abst. 10. 4-76.) -Authors' abstract.

D-410 Kraus, J. D. and Crone, W. Reed (both. Radio Obs. , Ohio

State Univ. ), Apparent observations of solar corpuscular

clouds by direct continuous wave reflexion. Nature, London, 184(4691) :965-966, Sept. 26, 1959. 2 figs. , 5 refs.

DWB--A paper reporting the details of several unique Doppler signals recorded at the Ohio State University Radio

Observatory on the morning of April 15, 1959. It is held

that the signals may possibly be due to the reflection of

continuous wave signals from fast moving solar corpuscular

clouds passing in the vicinity of the Earth. Instrumental details of the receiver and particulars of recordings are given.

Two photographs of swept frequency record of Doppler signals at different times are shown. A large solar flare which

occurred on April 13, and a number of terrestrial phenomena

occurring on April 15 are noted as suggestive of Doppler re- flections from solar corpuscular clouds. (Met. Abst. 12.4-

117. )- -Authors' abstract.

D-411 Kraus, J. D. ; Higgy, Robert C. ; Scheer, Donald J. et al.

(all, Radio Obs. Ohio State Univ., Columbus, Ohio),

Observations of ionization induced by artificial earth satellites . Nature, London, 185(4712) :520-521, Feb. 20, 1960.

2 figs. , 4 refs. DWB--While monitoring a remote CW station at the Ohio State Univ. it was found that large enhancements of signals often occur at the times near approach of

an artificial earth satellite. The enhancements are of such

145
magnitude as to indicate extensive ionization with scattering cross section several orders of magnitude greater than

the physical cross section of the satellite. A possible hypothesis is that the satellite encountered regions of high

particle density in the auroral zone scattering material into

ionized clouds or streams which travelled closer to columns

with reflections from these clouds causing many of the observed signals enhancements. While signals from the satellite dropped to a very low level for about 1 min, then rose

again, the decrease in signal coincided with the beginning

of the radar traces suggesting the possibility that the ionized particles encounters or produced at this time resulted

in absorption or scattering of the signal from the satellite,

while the particles acted as reflecting or back scattering

medium for the radar signals. (Met. Abst. unpub. )--

£. Z. S.

D-412 Kraus, J. D. ; Higgy, R.C. and Crone, W. R. , The satellite ionization phenomenon. Institute of Radio Engineers,

N. Y. , Proceedings, 48(4):672-678, April 1960. 5 figs.

,

table, 7 refs. DLC--A number of observations are presented

which show a close correlation between CW reflected HF

signals and passes of artificial earth satellites. The periodic (nonrandom) occurrence of the signal bursts and the

symmetry of some burst sequences are indicative of satellite related phenomena. The occurrence of a variety of satellite related Doppler effects are described and several satellite ionization mechanisms are also discussed. The possible relation of the satellite phenomenon to prior solar activity is mentioned. (Met. Abst. 12. 6-106. )--Authors'

abstract.

D-413 Kraus, J. D. (Radio Obs. , Ohio State Univ. , Columbus),

Apparent radio radiation at 11 m wavelength from Venus.

Nature, London, 186(4723) :462# May 7, 1960. 3 refs. DWB

--A critical review of preliminary communications referring

to the reception of 11 m radiation from the planet Venus in

1956. The author's conclusion is that to determine the ex- istence or nonexistence of such radiation beyond any doubt,

further observations are needed using a better equipment

than was available in 1956. (Met. Abst. 11. 12-65. )--E.K.

D-414 Kraus, J. D. (Ohio State Univ. Radio Obs. , Columbus),

Evidence of satellite induced ionization effects between

hemispheres. Institute of Radio Engineers, N. Y. , Proceedings, 48(11): 1913-1914, Nov. 1960. 2 figs., 10 foot-refs.

DWB--The sporadic ionization observed at a remote CW station at the Ohio State Univ. Radio Observatory, Columbus,

and monitored at the 330 mi distant WWV station near Washington, D. C. , is shown in a graph as a function of time

146
before and after near approach of Sputnik III on 14 nights,

Jan. -Feb. 1959 (50 passes). The larger peaks are shown

to coincide with the satellite's passage through the north- ern horns of the outer Van Allen belt and auroral zone. Apparent presence of high electron density (cloud) between the

satellite and the Columbus station may well be responsible

for the signal blocking there, while the WWV reflections

are increased. The situation is plotted on a map as observed on the night Aug. 9-10, 1959. Plausible explanations

for interhemispheric effects are also given. --W. N.

D-415 Kraus, J. D. and Higgy, R.C. (Radio Obs. , Dept. of Elec.

Engr. , Ohio State Univ. , Columbus, Ohio), The relation of

the satellite ionization •phenomenon to the radiation belts.

Institute of Radio Engineers, N. Y. , Proceedings, 48(12):

2027-2028, Dec. 1960. 3 figs. , 5 refs. DLC--A telemetering equipment located at the Ohio State Univ. Radio Obs. , has been used during March and April 1960 to monitor the

Explorer VII transmitter (19. 991 Mc ) and its counting rates

of the Antom 112 and 302 Geiger counters: The observations revealed that many of the strongest enhancements of

signals from WWV (located near Washington, D.C. ) occurr- ed very close to the time when the counting rates of the

Geiger counter aboard Explorer VII were at peak values.

These events were also accompanied by a partial or complete fadeout of the signal from the satellite. The signal

"drop-outs" suggest the existence of ionization patches or clouds between the satellite and Columbus. These clouds

attenuate the signal from the satellite transmitter and at the

same time act as reflecting or back scattering regions for

the WWV signals. A typical observation of these effects

is discussed as observed on March 30, 1960. It is also

noted that this ionization may be induced by the satellite

in the most tense part of the radiation belt, due to encounters between the satellite and the regions of high particle

density and/or energy. (Met. Abst. 13A-104. )«N. N.

D-416 Krishnamurthi, M. ; Sivarama Sastry, G. and Seshagiri Rao,

T. (all, Physical Laboratories, Osmania Univ. , Hyderabad),

Abnormal ionospheric behaviour at 10 metres wavelength.

Current Science, Bangalore, 27(9):332-333, Sept. 1958. fig.,

table, ref. DLC—The radiation intensity of 10 m cosmic

radio waves fell to zero on Jan. 28, Feb. 21, and March 2,

1958 at the Physical Laboratories, Osmania Univ. , Hyderabad, India (17°26' N, 78°27' E). The gradual fall of intensity occurred about sunrise time, and the rise of intensity

toward end of the phenomenon was uniformly rapid in the

three cases, but differed in duration of minimum noise level.

147
Small scale irregularity in the upper ionospheric layers is

offered as a plausible cause of this disturbance which is

knowingly unrelated to any solar flare. (Met. Abst. 11E82. )-W. N.

D-417 Krishnan, T. and Mullaly, R.F. (both, Radiophysics Lab.,

CSIRO, Sydney), Decimeter radio bursts concurrent with

solar Type IV radiation . Nature, London, 192(4797): 58-59,

Oct. 7, 1961. fig., 2 refs. DWB, DLC -Observations of

1.420 Mc/s solar radio bursts have been made using a Christiansen crossed grating interferometer. Eight occasions characterized by intense type IV activity have been

chosen for detailed analysis. The meter wave length

sources were located in the high corona, the 1.420 Mc/s

sources remained at rest in the chromosphere or lower cor- ona not more than 50, 000 km above the H &• flares. The

low frequency sources, on two occasions, showed large

scale movements while the decimeter source was stationary. It was concluded that the decimeter burst and the

meter wavelength type IV source must be different. --R.B.

D-418 Krivsky, L. (Astrophys. Obs. , Ondrejov), Ausserunq der

chromospharischen Eruptionen in den atmospharischen St6r- ungen. (Manifestation of chromospheric eruptions in atmospheric disturbances.) Bulletin of the Astronomical Institutes of Czechoslovakia, Prague, 4(S):196, 1953. tables.

DLC --Correlations between chromospheric eruptions of importance 1, 2 and 3, and sferics on 11 km wavelength were

statistically analyzed for the period July 1951-Sept. 1952.

General results of the analysis are tabulated and briefly

commented on. (Met. Abst. 8. 1-390. )--G.T.

D-419 Kuiper, Gerard Peter (ed. ), The sun. Chicago, Univ. of

Chicago Press, 1953. 745 p. numerous figs., (incl. photos),

tables, eqs. Bibliogs. at end of most chapters or sections.

DV/B--This is Vol. 1 of a series of four volumes on The solar

system. The second volume is The earth as a planet, the

third Planets and comets. The present volume contains the

following chapters: I. Introduction, by Leo Goldberg (historical solar constants, solar physics, solar terrestrial re- lationships, solar atmosphere); II. The sun as a star, by

Bengt Stromgren; III. The photosphere, by M. Minnaert; IV. The identification of solar lines, by Charlotte E. Moore;

V. The chromosphere and the corona, by H. C. van de Hulst;

VI. Solar activity, by K. O. Kiepenheuer ;VII. Solar radio

emission, by J. L. Pawsey and S. F. Smerd; VIII. Solar electrodynamics, by T. G. Cowling; IX. Empirical problems and

equipment, by C. W. Allen, P. C.Kunan, R. R. McMath, J. W.

Evans, W.O.Roberts, R.Tousey, J. G. Wild, H. W. Dodson,

A.Ehmert, J.A.Simpson and others. The entire range of

148
subjects in the field of astrophysics is included: for instance, measurement of solar constant, the zodiacal light,

ionosphere during eclipses, rocket observations of UV;

extreme UV and X-rays, radio frequency radiation from sun,

solar flares, 200 cm/sec radiation, cosmic rays from sun,

Alfven's theory of magnetic field in sunspots, corpuscular

streams, auroras; and of course, historical and bibliographic material; tables of constants, etc. (Met. Abst. 11A-63. ) --M.R.

D-420 Kundu, Mukul Ranjan, Etude des sources solaires persist- antes sur ondes centimetriques . (Study of the persistent

solar sources on centimetric waves.) Academie des Sciences, Paris, Comptes Rendus, 246(19): 2740-2743, May 12,

1958. 3 figs. , 4 refs. DLC--The author uses an interferometer with two antennas, the effective inter fringe of which

increases in accordance with the horary angle of the observed heavenly body. This apparatus, which operates on 3. 2

cm wavelength, has been used to study the passably stable

emission sources located in the solar atmosphere. Measurements of brilliancy distribution of the persistent solar

sources on centimetric waves indicate that certain sources

are intense and narrow (diameter about 1'5), others are less

brilliant and more extended. It is discovered that the appearance of the narrow sources is connected with the periods of eruptive activity of the sun. (Met. Abst. unpub. )--

A.V.

D-421 Kundu, Mukul Ranjan, Sur les dimensions des sources des

sursauts de rayonnement solaire sur les ondes centimetriques. (The sizes of the solar radiation jumps sources on

centimetric waves.) Academie des Sciences, Paris, Comptes Rendus, 246(20): 2852-2855, May 19, 1958. fig. , 7

refs. DLC --Measurements of the sizes of jumps sources

made with an interferometer have made it possible to specify the classification of jumps, to follow up their evolution

in size and to value their equivalent temperature. The

equivalent temperature of some jumps observed on centimetric waves may reach several tens of millions of degrees;

it is thus highly probable that they are not of thermic origin, a conclusion which is in agreement with the observations of

jumps, made in the field of metric waves. (Met. Abst.

unpub. )--A. V.

D-422 Kundu, M. R. and Denisse, J. F. , Solar radiation on decimeter waves as an index for ionospheric studies . Journal of

Atmospheric and Terrestrial Physics, London, 13(1/2):176-

178, Dec. 1958. 2 figs. , 5 refs. DLC --The probability of

obtaining an index of solar activity useful for ionospheric

studies for shorter periods than a month by the intensity of

149
solar radiation on decimeter waves is indicated. The presented correlation diagrams of monthly and of 5 day mean

values illustrate that the 10. 7 cm solar flare radiation density F should be adopted in the place of the Wolf number R

for most ionospheric studies. (Met. Abst. unpub. )--0. T.

D-423 Kundu, M. R. , Structures et proprietes des sources d'acti - vite solaire sur ondes centimetrigues. (Structures and properties of solar activity sources on centimeter waves.)

Annales d'Astrophysique, Paris, 22(1):1-100, Jan. /Feb.

1959. numerous figs., tables, eqs., 41 refs. French,

English and Russian summaries p. 1. DWB, DLC--A twoantenna interferometer has been constructed for the study of

localized sources on the sun (persistent sources and bursts)

on centimeter waves (3.23 um)= The two antennas are in

equatorial mounting and are placed on an E-W base line at a distance of 60 m from each other. The variation of the re- solving power due to the diurnal motion is utilized to measure the dimensions and distribution of brightness of these

sources. Observations with this instrument have brought

new evidence on several properties of these sources: evolution, apparent diameter, polarization, etc. , which clarify

considerably their classification and give new clues to their

interpretations and their association with the corresponding

phenomena observed in optics and on decimeter and meter

waves. We have also been able to show an extremely close

relationship between the ionization of the E layer of the ionosphere and 10-7 cm solar radiation. (Met. Abst. 11D-76.

)

—Author's abstract.

D-424 Kundu, M. R. and Haddock, F.T. (both, Univ. of Mich.

Obs. , Ann Arbor), A relation between solar radio emission

and polar cap absorption of cosmic noise. Nature, London,

186(4725) :610-613, May 21, 1960. 3 figs. , 3 tables, 7

refs. DW6--A statistical study of the nature of centimeter

and meter wave solar radio outbursts associated with polar

cap absorption and a general conclusion for the prediction

of proton events is presented. An analysis of 31 events of

polar cap absorption, illustrated by tables and diagrams,

shows a close correlation between the presence on the sun

of the sources of broad band centimeter wave outbursts or Type IV events, and the probability that these "active re- gions" play some part in the storage or trapping of the protons responsible for absorption events in the polar regions.

(Met. Abst. 11L-102.)-O.T.

150
D-425 Kuperov, L.P. , Nabliudeniia za signalami tret'ego sovetskogo iskusstvennogo sputnika Zemli na myse Cheliuskina . (Observations of the signals of the third Soviet artificial

earth satellite on Cape Chelyuskin. ) Iskusstvennye Sputniki Zemli, Moscow, No. 5:66-70, 1960. fig. , table. DLC

—Oscillograph recordings of the Sputnik Ill's radio signals

were made by members of the Arctic and Antarctic Scientific

Research Institute during the period May 16 to June 6, 1958.

The 20. 005 Kc receiver described, was turned on a few

minutes before the satellite appeared and remained on until

the signals faded out (10-15 min). The satellite transmitted

signals varied with the ionospheric conditions. Tabulated

results according to visible and non-visible satellite position above and below F2 are presented and isoline plottings

are shown on a northern hemisphere map. (Met. Abst. un- pub. )--N.P.S.

D-426 Kurnosova, L.V.; Razorenov, L.A. and Fradkin, M.I.

Kosmicheskoe izluchenie Solntsa . (Cosmic radiation from

the sun. ) Priroda, Moscow, No. 1:94-96, Jan. 1961. 2

figs. , 2 refs. DLC--The second cosmic rocket of the U.S.

S. R. contained two Cherenkov counters. These recorded on

Sept. 12, 1959, 11:27 o'clock, world time, an increase of

11. 8 times in the number of nuclei with the atomic number

15. This increase lasted 17 min. At the same time the

total number of nuclei with Z> 2. and 7L

^ 5 rose

only 1. 3 + 0. 1 and 1. 5 + 0. 3 times; the rise in the number

of the latter was almost entirely due to nuclei withZ ^ 15 . During the time corresponding to this short period increase

in the intensity of nuclear components there were recorded

two chromospheric flares of class I, which began at 11:36

o'clock and 11:39 o'clock, with heliographic coordinates of

21 N, 38 z. and 19 N and 33 E, respectively; the latter was

near a small sunspot. Since the number of weak chromosphere flares is considerable there is a high probability that

the observed increase coincided accidentally with such

flares. A more likely relationship to the increased intensity of nuclear components is attributable to the burst of

radiowave radiation which occurred on Sept. 12, 1959, at

11:29 o'clock; the intensity was 810 MHz and lasted less

than 0. 3 min. The probability of accidental coincidence of

this burst with the increased intensity of nuclear components

is less than 1%. Two more cases of increased intensity of

nuclei streams with ~Z- ^ \5 were recorded on Sept. 12,

1959 at 12:37 o'clock and 15:23 o'clock; the former lasted

13 min and the latter 25 min. The probability that this phenomenon was associated with statistical fluctuations was

3 X 10"3 . Both variations occurred during chromospheric

flares which were in the vicinity of a large group of sunspots. No special features of radio radiation were observed

151
with these phenomena. The characteristic short period increase in streams of nuclei of cosmic rays indicates that

there occur solar processes in which the nuclei are accelerated up to energies exceeding 1. 5 X 10^ £,v/nucleon,

since largely more heavy nuclei are accelerated. --I.L.D.

D-427 Kurnosova, L.V., Nekotorye rezul'taty issledovanii pri

pomoshchi iskusstvennykh sputnikov Zemli. (Some results

of investigation with the 3rd artificial earth satellite.

)

Priroda, Moscow, No. 6:85-86, June 1958. fig. DLC.

Transl. into English by E. R. Hope issued as Canada. Defence Research Board, Translation T-304-R, Sept. 1958.

2 p. typescript. DWB--Satellite data on the intensity of

cosmic radiation showed that up to 700 km the intensity

increased up to 40% in comparison with that observed at

200 km. The intensity above 200 km increases because of

two reasons, namely: with increasing height the "screening"

action of the earth decreases, and since cosmic rays are propagated in space isotropically a recording device in

space records considerably more than one near the earth;

also the higher the elevation the more particles can penetrate the magnetic field of the earth, which exerts a deflecting action upon cosmic particles and this effect is more intense the closer they are to the earth. The line of equal intensity of cosmic rays does not coincide with the geomagnetic parallels. During the flight of the earth satellite the

halogen counters recorded short period, abrupt variations

in the intensity of the cosmic rays, while such variations

were not observed at the surface of the earth. (Met. Abst.

12. 5-118. )--I„L D.

D-428 Laffineur, M. , Correlation entre certains phenomenes qeophysiques et le rayonnement solaire sur 55 cm. (Correlation between certain geophysical phenomena and solar radiation at 55 cm.) International Council of Scientific Unions,

Brussels, Commission for the Study of Solar and Terrestrial

Relationships, Rome, Sept. 1952, Report No. 8:19-20, pub.

1953. fig. , table. DWB--Disturbances on 55 cm occur as

"points" or as bursts but not as storm noise. Radio electric phenomena accompanying chromospheric eruptions are tabulated under intense and weak points and intense and

weak bursts (of 1-90 minutes). (Met. Abst. 5. 8-266. )--

C.E. P, B.

D-429 Laffineur, M. , La radio-astronomie se developpe. (The

development of radio astronomy.) L'Astronomie, Paris,

p. 179-191, May 1953. figs., photos, foot-refs. DWB--

Advances made in radio astronomy during 1952 are outlined

and discussed, including mention of conferences in Australia, Rome and Paris. Solar radio radiation from a calm

152
sun, a disturbed sun, intense eruptions, eclipses, etc. , are discussed and the equipment used in various places

for measuring these radiations illustrated. Emissions from

stars, galaxies and interstellar space are also discussed.

Finally, interferometry and ionospheric radio astronomy are

treated. Mitra and others showed how the ion density in

the ionosphere could be calculated by measuring the decrease in galactic noise. At Meudon, France, continuous

records of galactic radiation at decameter wavelengths have

been made. (Met. Abst. unpub. )--M. R.

D-430 Laffineur, M. and Whitehead, J. D. , The measurement of

cosmic radio emission for ionospheric studies . Journal of

Atmospheric and Terrestrial Physics, 9(5/6) :347-349, Nov.

1956. 2 figs., ref. DWB--A technique is described, in

use at Meudon Observatory near Paris, for recording automatically cosmic noise from the Cassiopeia source on 24

Mc/s - 24. 1 Mc/s, in spite of severe local interference.

Some records are shown. (Met. Abst. 8. 4-124. )--C.E. P.B.

D-431 Laffineur, M. , Radio-astronomie . (Radio astronomy.

L'Astronomie, Paris, 72(5): 209-214, May 1958. 2 figs.

DLC --Radio astronomy, science of observation of matter in

the dilute state, makes a great contribution to the enlightenment of our knowledge of the Universe. In order to encourage students to take interest in this new science, the author summarizes succinctly some important points, particularly: the visual sky and the radioelectric sky, the nature

of the observed radiation, the intensity of the received ra- diation. He illustrates his article with the telemetry of our Galaxy. The end of the article deals with galactic hydrogen

and its emission on 21 cm, the Doppler-Fizeau effect and

radio sources. (Met. Abst. 11. 5-159. )--A. V.

D-432 Laffineur, M. , La radioastronomie. (Radio astronomy.

Revue Generale des Sciences Pures et Appliquees, Paris,

66(3/4): 79-86, March/April 1959. DLC -After a short re- view of K.JANSKY's experiments, the difference between

optical astronomy and radio astronomy is pointed out as well

as the advantages and disadvantages of each of these sciences. -This article constitutes a synthesis of the contributions made in recent years by radio astronomy to our knowledge of the Universe. Author considers particularly the following subjects: solar emission, telemetry of our galaxy,

galactic hydrogen and its emission on 21 cm, Doppler-Fizeau effect and radio sources. (Met. Abst. 11. 5-160. )--A.V.

153
D-433 Landmark, B. ; Lied, F. ; Orhaug, T. and Skribeland, S.

,

Ionospheric observations during the solar eclipse of June

30. 1954. Geofysiske Publikasjoner, Oslo, 19(8), 1956.

39 p. 22 figs. , 2+ tables, 3 refs. , eqs. DLC --This monograph consists of 3 parts: Pt. I, by LANDMARK, LIED and

SKRIBELAND, discusses and presents data on h'f observations obtained during the eclipse of June 30, 1954 at the

3 NDRE stations. It is shown that the F2 layer observations

at time of total eclipse can only be explained by a definite

solar control over the ionizing agency. Recombination coefficients have been worked out for the E, Fl and F2 layers.

Pt. II, by LIED and ORHAUG, on Fl layer ionospheric absorption during the eclipse is based on observations at

Kjeller and Tromoya, especially those made with variable

frequency equipment, gave a basis for a solar "model".

Pt. Ill, by LIED, on "an ionospheric layer during a solar

eclipse" shows electron density profiles and other characteristics of an eclipse ionospheric layer. (Met. Abst. 11F71.)-M.R.

D-434 Lange -Hesse, Gunther, Variation der brauchbaren Taqesfreguenzen im Kurzwellenweitverkehr als Wirkunq solarer

Partikelstrahlung. (Variation of the diurnal useful frequencies used in shortwave long distance communication as an

effect of solar corpuscular radiation. ) Archiv der Elektrischen Ubertragung, Stuttgart, 14(3): 115-120, March 1960.

4 figs. , 12 refs. German and English summaries p. 115.

DLC --The observational data of the ionospheric station

Lindau/Harz ( Q£3£ 52 ) and the geomagnetic observatory

Wingst ( <£ £^r 54 ) is analyzed in order to find the statistical relation between the degree of geomagnetic activity

as a measure for the intensity of the incident solar particle

radiation and the relative deviations of the factor M 3000

and the MUF3000 from their median values (M3000 conversion factor from vertical to oblique incidence critical frequency for 3000 km distance, MUF 3000 maximal usable frequency for 3000 km distance). The observational data are ar- ranged only according to the degree of geomagnetic activity,

then following average behavior of M 3000 and MUF 3000 is

determined for the different degrees of geomagnetic activity.

In the statistical relationship there is a distinct dependence

on the sunspot cycle and the seasons. The practical significance of these results is discussed in detail with respect

to the prediction of disturbances in short wave propagation

conditions. The investigations are also a contribution to

the study programmes No. 93 (VI) and No. 150 (VI) again

proposed at the last CCIR-Planary Assembly (Los Angeles

1959). (Met. Abst. 11. 12-130. ) -Author's abstract.

154
D-435 Lauter, Ernst August (Met. Obs. , Kuhlungsborn, Germany),

Measurements on medium and low frequencies and of atmospheric noise during the solar eclipse of June 30, 1954. (In:

Solar eclipses and the ionosphere: a symposium. . . ed. by

W. J. G. Beynon and G. M. Brown. London, Pergamon, 1956.

p. 124-125! ) DWB (523. 7 S684)- -Eel ipse effects on the intensity of sky-waves received on various frequencies at distances varying from 180 to 700 km are described. The dependence of the duration of the effect (delayed start and premature ending relative to the eclipse) on frequency and distance can be interpreted in terms of a simple D region of

double structure. Atmospheric noise measurements on 8 to

69 kc/s indicate an increase up to the eclipse maximum (depending on frequency and distance) and a steep decrease

afterwards. (Met. Abst. 9A-122. )--Author's abstract.

D-436 Lauter, E. A. ; Bartels, G. ; Sprenger, K. and Skeib, G.

,

Per Intensitcittsanstieq der kosmischen Strahlung am 23. 2

1956 und qleichzeitige Effekte in der tiefen Ionosphare.

(The increase of intensity of cosmic radiation on Feb. 23,

1956 and simultaneous effects in the lower ionosphere. ) Zeitschrift fur Meteorologie, 10(5): 129-131, May 1956. fig.,

3 refs. DLC--The increase of cosmic radiation shown by

observations at Ktfhlingsborn began at 0342 GMT and by 4-

5 h exceeded 65%, the limit of the electrometer; it probably

reached 150%. It powerfully affected long wave transmission (35-40 kHz) in the nocturnal D region. Disturbances

on 40-5 kHz at Kuhlingsborn and Potsdam are shown graphically. On 185 kHz there was a sudden increase of absorption at 0348 GMT which continued to midday, also found on

245 and 1178 kHz. Next day there was an intensity rise of

6. 2 % at 12-13 h. (Met. Abst. 8. 1-181. )-C. E. P. B.

D-437 Lauter, E. A. and Triska, P. , Zur Deutunq der plotzlichen

Feldanomalien im Lanqwellenbereich bei Sonneneruptions - effekten. (Interpretation of sudden field anomalies in long

wave communication due to solar eruption effects.) Zeitschrift ftfr Meteorologie, Berlin, 13(7/8): 190-192, July/Aug.

1959. 3 figs., 2 refs. DWB, DLC -The basic characteristics

of the phenomenon are described as due to phase alterations

between surface and space waves caused by sinking of the re- flection level as shown by simultaneous measurements at the

observatory Kfthlungsborn and at the Geophys. Inst. , Czechoslovak Acad, of Sci. at Prague, of transmissions from Brasow, at a distance of 1360 km. The analysis of the apparent

height alterations on the basis of an equation of geometric

optical extensions between surface and space waves proved

the existence of a solar eruption effect in the lower ionosphere as well as the variations of the apparent reflection

level. These and some other results of the analysis are

155
illustrated by diagrams of recordings of electric field

strength height variations of the apparent reflection level;

of the analysis of the apparent reflection level associated

with stronger solar eruption effects; and of the distribution

of characteristic parameters of solar eruption effects. (Met.

Abst. 11. 10-47. )--O.T.

D-438 Lawrence, Lovell, Jr. , "Astro"- -an artificial celestial navigation system. Franklin Institute, Phila. , Journal of the

Franklin Institute Monographs, No. 2:89-99, June 1956.

table, 7 refs. , 7 figs. DWB—This paper treats the peaceful use of "Astro", an Artificial Satellite Time and Radio

Orbit* to be established over the earth for celestial navigation purposes. Every effort has been made to create a simple, yet reliable, system that may be feasible in the near

future. To accomplish this, however, a very high degree

of accuracy must be maintained in the electronic components. Methods for observing this high velocity body by

other than optical means will be necessary, and accurate

time signals must be generated. The selection of 105 min

polar orbits versus 24 hr orbits will be discussed, and some

consideration will be given to the design of the Astro Satellite--including methods for propagating electromagnetic

wave signals of one hundred megacycles --together with a re- view of a nuclear power source for supplying the necessary

electrical energy. Reference will be made to the standard

celestial navigation techniques, using circles of equal altitude obtained from an electronic sextant. To establish a

fix, an arrangement will be explained for obtaining lines of

position by interpreting observed Doppler frequency deviation versus position distance from the satellite. A graph of

this Doppler shift, and a Mercator position plotting sheet

will be used to describe a typical aircraft flight. (Met. Abst.

8. 11-71. ) -Author's abstract.

D-439 Lawrence, L. , Jr. , Navigation by satellites . Missiles and

Rockets, Wash., D.C., l(l):48-52, Oct. 1956. 8 figs.

DLC --Detailed review of a system for ship navigation by

earth satellite fixes. (Met. Abst. 9. 10-120. )--M. R.

D-440 Lawrence, Robert S. (Nat'l. Bureau of Standards, Boulder,

Colo. ), An investigation of the perturbations imposed upon

radio waves penetrating the ionosphere . Institute of Radio

Engineers, N. Y. , Proceedings, 46(1): 315-320, Jan. 1958.

4 figs. , 38 refs. DLC--A new method has been devised to

measure continuously the phase deviations introduced by

the ionosphere into the signals from discrete sources. Sample recordings of measurements at frequencies of 53, 108,

and 470 Mc are given. An experiment combining this phase

measuring technique and standard ionospheric soundings at

156
the point of penetration of the line of sight is in progress

and is expected to shed light upon the height of origin of

ionospheric scintillations. (Met. Abst. 1 IE -84. )- -Author's

abstract.

D-441 Lawrence, R.S. and Jespersen, James L. , A preliminary

analysis of amplitude scintillations of radio stars observed

at Boulder. Colorado. U.S. National Bureau of Standards,

Technical Note, No. 20, July 1959. 19 p. 9 figs., table,

20 refs. , 17 eqs. DWB (M(055) U585te) -Variations in the

apparent flux from the radio source Cygnus-A are recorded

at 53 and 108 mc/s using a two element phase sweeping interferometer located at Boulder. An ionospheric sounder

operating at Ellsworth, Nebraska, provides simultaneous

vertical incidence measurements of the ionosphere along the

path. Amplitude scintillations observed at Boulder over a six month period are compared with the ionograms taken at

Ellsworth. Positive correlation is found between amplitude

scintillations and spread F, while a small negative correlation is found with sporadic E. The present result appears

to be significant but a full year's data are being accumulated to disclose seasonal or diurnal effects. Detailed an- alysis of the scintillations indicates that the probability distribution of the amplitude can be represented by the Rice probability distribution function. The scintillation rate for 108

Mc/s seems to be more rapid than for 53Mc/s. (Met. Abst.

11F-74. )--Authors' abstract.

D-442 Lawrence, R.S., Ionospheric scintillation of radio waves

of- extraterrestrial origin. (In: Menzel, Donald H. , ed. ,The

Radio Noise Spectrum. Cambridge, Mass. , Harvard Univ.

Press, 1960. p. 43-47. 2 figs. , 3 refs.) DWB--A brief re- port of work in progress at Boulder, Colorado. Phase scintillations are measured by means of a phase tracking and

phase sweeping interferometer. This instrument can be used

in its phase tracking mode to provide a continuous record of

phase scintillations, or it can be used with phase sweeping

to provide a record from which amplitude and phase information can be extracted independently. At this time, it is not

certain whether the diffraction responsible for any particular

scintillation record occurs at a height of 100 or 400 km or at

intermediate heights. The present experiment at Boulder is

an attempt to clarify this question. Each day, soon after

the rise of Cygnus A above the northeast horizon ionospheric

pulse soundings are made with a sweep frequency vertical incidence sounder 300 km away in Nebraska. The sounder is

so placed as to observe the very portion of the ionosphere

which causes the scintillations recorded at Boulder. Comparison between these two methods of observing the ionosphere has verified the previously reported relation between

157
scintillations and spread Ff and strongly suggests an inverse relation between scintillation and sporadic E. If

further investigation corroborates this relation, we will

have definite knowledge that some of the scintillation activity arises at the 100 km height of the E region. Some

amplitude and phase scintillation records are shown. (Met.

Abst. unpub. )--E. Z. S.

D-443 Lawrence, R.S. and Little, C.G. (both, Boulder, Colo.),

On the analysis of polarization rotation recordings of satellite signals . (In: International Scientific Radio Union, IGY

Committee, Some ionospheric results obtained during the

IGY. Amsterdam, Elsevier, 1961. p. 391-399. 7 figs.

,

4 refs. , 3 eqs. PLC--A method is presented which permits

accurate estimates of the total electron content below the

satellite height from observations at 20 Mc and rejects simplifying assumptions of ionospheric rotation of the polarization plane of a satellite radio signal. The derived analyses

permit the study of ionospheric tilts and have revealed large

scale irregularities in the ionospheric electron content. The

deviation in sub-satellite content of these irregularities is

of the order of 2% of the running mean values; the lateral extent of irregularities is of several hundred kilometers. The

effect of such irregularities upon ionospheric refraction and

satellite Doppler curves are discussed. (Met. Abst. un- pub. )--S.N.

D-444 Leadabrand, Ray L. (Stanford Res. Inst., Menlo Pk. , Calif.),

Radar Astronomy Symposium report. Journal of Geophysical

Research, Wash., D.C., 65(4):1103-1118, April 1960. 12

figs. , 14 refs. DLC--The purpose of the Symposium held in

San Diego, Oct. 1959, by the U.S. National Committee of

the International Scientific Radio Union, was to call attention to the potential usefulness of radar in the exploration

of the solar system and to report on past work. The following topics were included: radar studies of the moon; planets;

exosphere and the interplanetary medium — Sun, meteors and

auroras. The members of the panel made a progress report in

each field and indicated the potentialities for future research

The radar approach to astronomical studies in the solar system is fundamentally complementary to passive visual and

radio astronomy. (Met. Abst. U. 12-75. )--E. Z. S.

D-445 Leadabrand, R.L. ; Dyce, R.B. ; Fredriksen, A. et al.

(all, Stanford Res. Inst., Menlo Park, Calif.), Radio frequency scattering from the surface of the moon. Institute of

Radio Engineers, N. Y. , Proceedings, 48(5): 932-933, May

1960. 3 figs., table, 7 refs. DLC--The moon, observed

with two high powered 4000 Mc radars, one located at College, Alaska, and the other at Fraserburgh, Scotland, was

158
D-446

D-447

D-448

D-449

found to behave as a smooth reflector as well as a diffuse

scatterer. The image of the moon, as it would appear to

the observer, utilizing the range increment and the Doppler

shift increment, is reproduced as a number of concentric

rings. --W. N.

Lebedeva, P. N. ; Neishild, V. G. and Panovkin, B. N.

,

Radioastronomiia. Annotirovannii bibliograficheskii ukazatel otechestvennoi i inostrannoi literaturi, 1932-1958 gg.

(Radio astronomy. Annotated bibliographical index of

native and foreign literature, 1932-1958. ) Academy of Sciences of the U.S.S. R. Section: Network of special libraries. Library of the N. P.Lebedeve Physical Institute. 216 p.

--The material is grouped under the following sections: (1)

Methods of radioastronomy. (2) Solar, lunar and planetary

radio emanation. (3) Galaxy and metagalaxy radio emanation. (4) Concealed sources of radio emanation. (5) Monochromatic emanation of the galaxy. (6) Study of the earth's

atmosphere through radioastronomic methods. (7) Reviews,

(unchecked. )--W. N.

Lee, Robert H. , Solar flare detection for I. G. Y. Electronics, 30(3):162-165, March 1957. 6 figs. , 2 refs. -Two re- ceivers detect changes in D layer as indicated by increased

atmospheric signal at 27 Kc/s and decreased cosmic noise

signal at 18 Mc/s. --CSIRO Abstract.

Lehigh University. Institute of Research, Absorption of

microwaves in gases . Contract AF 19(1222) -2, Progress

Report, Nos. 9 and 10, Sept. 30, 1951. 10+ p. 2 tables,

8 figs., foot-refs. DWB--Very detailed description of the instrumentation used in the dynamic method developed to re- cord the semi-log plot of the Volt-Ampere characteristics of a probe. The method explained greatly facilitates investigation of electron temperatures; for which density tables are presented. (Met. Abst. unpub. )--W. N.

Lehnert, Bo Peter (ed. ), Electromagnetic phenomena in cosmical physics. Cambridge, Univ. Press, 1958. 544 p.

bibliogs. Price: 50 sh. (International Astronomical Union,

Symposium, No. 6, held in Stockholm, Aug. 1956. (Pertinent articles abstracted separately. ) DLC (QB461.L43)--

A collection of 56 articles on magneto hydrodynamics (theory,

experiments and observed behavior of ionized gas in a magnetic field), solar electrodynamics, stellar magnetism, solar

and interplanetary magnetic fields, electromagnetic state in

interplanetary space (magnetic storms and cosmic ray behavior), high current discharges and radio astronomy, etc. , read

at the 6th International Astronomical Union Symposium held

159
in Stockholm, Aug. 27, 1956, under the general chairmanship of H. ALFVEN. Articles include discussions. (Met.

Abst. 11.5-27. )--M.R.

D-450 Leighton, Hope I. (Nat'l. Bur. of Stands. , Boulder, Colo.),

Field strength variations recorded on a VHF ionospheric

scatter circuit during the solar event of Feb. 23. 1956.

Journal of Geophysical Research, Wash., D. C, 62(3):

483-434, Sept. 1957. fig. DLC -Field strength anomalies

of the SID type from 0300 to 1000 h Feb. 23, 1956 on 49. 8

Mc (Cedar Rapids to Sterling) are shown graphically. Time

coincided closely with flares seen at Tokyo and Kodaikanal

and cosmic ray outbursts reported from all over the world.

Rise in signal strength coincided with onset of flare, maximum anomaly with maximum intensity of cosmic ray enhancement, and return to normal signal strength with end of SID

as reported from Okinawa and Japan, but continued after end

of solar flare. (Met. Abst. 11E-85. )--M. R.

D-451 Lejay, Pierre, Methodes modernes de recherches sur la

haute atmosphere . (Modern methods of research on the upper atmosphere.) Conference at the Palais de la Decouverte,

Jan. 16, 1954. Paris, 1954. 25 p. 5 figs. (Conferences

du Palais de la Decouverte, Ser. A, No. 192. ) DLC--Spec - troscopic rocket (direct measurement) and radio echo methods of upper atmospheric research are described, and results

in terms of temperature (to 150 km), density, winds, ionization, chemical composition, oscillations and radio propagation conditions discussed in this pamphlet. (Met. Abst.

12E-68.)--M.R.

D-452 Lepineux, M. , Discrimination des eruptions chromospher- iques associees aux perturbations geomagnetiques durant le

maximum solaire actuel. (Discrimination of chromosphere

eruptions associated with geomagnetic disturbances during

the present solar maximum. ) Academie des Sciences, Paris,

Comptes Rendus, 247(1):109-111, July 7, 1958. 2 tables,

5 refs. DLC—The author considers the period of the welldefined solar maximum from April 15, 1957, to March 31,

1958. He splits up the important chromosphere eruptions

into two categories. On the one hand, those which are ac- companied by a well marked and rather long lasting increase

of the radioelectric noise range on frequencies near 200 Mc/s.

These eruptions generally occur during a pre-falling of the

cosmic rays. Such eruptions determine, 20 to 70 hrs afterwards, a disturbance of the terrestrial magnetism, if they

happen sufficiently close to the center of the apparent disc.

On the other hand, those which are not accompanied by this

long increase of the radioelectric noise on 200 Mc/s, whatever their position and importance, are not associated with

geomagnetic disturbances. (Met. Abst. 10. 8-105. )--A. V.

160
D-453 Leslie, Patricia R.R. and Elsmore, B. (Mullard Radio Astronomy Obs. , Cambridge), Radio emission from the Perseus

cluster. The Observatory, London, 81(920):14-16, Feb. 1961.

2 figs. , table, 10 refs. --It has been suggested by J.B.BALDWIN and B. ELSMORE (Nature, 173, 818 (1954)) that 75% of

the radio emission from the Perseus cluster originates in NGC

1275, and the remainder from an extended source associated

with the cluster. Observations show that there are two components of small angular size. The positions and flux densities, together with angular diameter, as well as the optical

data for NGC 1275 and the cluster, are shown in a table. The

position and angular diameter of the strongest component are

in agreement with optical measurements of NGC 1275, while

the position of the extended source is close to that of the

center of the cluster, but neither its brightness, nor its integrated flux density agree with the figures computed on the supposition that the emission arises from a component member of

the cluster. The extended feature may be associated with the

presence of two sources of small angular size and might arise

in the manner proposed by I.S.SHKLOVSKY (see ref. D-750,

1955) (5th Conference on Cosmology, Moscow, p. 395 (1955))

from the interaction of the gaseous contents of two interacting

galaxies. (Met. Abst. 9A-46. )-S. N.

D-454 Lied, F. , Ionospheric absorption observed on Feb. 23, 1956

at Kieller and Tromso. Journal of Atmospheric and Terrestrial

Physics, 10(1):48, Jan. 1957. fig. , DWB--Records at Kjeller

shown during intense solar eruption of Feb. 23, 1956. Absorption increased gradually from 0400 GMT but echoes were not

lost. At Tromso echoes were lost. (Met. Abst. 8.6-185.)--

C.E.P.B.

D-455 Lied, F. (Norwegian Defence Res. Estab. ), Quantitative

measurements of absorption in the auroral zone. (In: Polar

Atmosphere Symposium, Oslo, July 2-8, 1956, Proceedings,

Pt. 2, Ionospheric Section. N. Y. , Pergamon Press, 1958.

p. 135-146. 14 figs., 11 refs.) Also issued in Journal of

Atmospheric and Terrestrial Physics, London, Special Supplement, Pt. 2, 1957, pub. 1958? p. 135-146. DLC--In the study

of "normal" auroral absorption as well as the disturbances, we

need the application of different techniques with overlapping

sensitivity since the observational phase in connection with

ionospheric absorption is not terminated. The statistical distribution in time and space of the more catastrophic blackouts,

a little of the real nature and cause of the general and excessive high absorption due to some ionizing mechanism, and the

techniques for locating where in the ionosphere the excessive

absorption takes place, as well as the magnitude of the extra

ionization, have been covered in this paper. Techniques include the CW oblique measuring, the pulse amplitude, the

161
Galactic, the cross modulation techniques, all of which must

be used contemporaneously and forced to overlap as in the

ionospheric recordings made in Canada, Alaska and Norway.

(Met. Abst. 10. 9-316. )--N. N.

D-456 Lilley, A. E. , The absorption of radio waves in space. Scientific American, 197(1) :48-55, July 1957. 9 figs. DWB,

DLC --Mostly about radio astronomical problems associated

with nonterrestrial absorption of hydrogen emissions. Radio

astronomers work mainly with hydrogen lines (21 cm), since

93% of all atoms in the universe are hydrogen. (Met. Abst.

9A-156. )--M. R.

D-457 Lincoln, J. Virginia, SID type phenomena and solar flares.

U. S. National Bureau of Standards, NBS Report, 5065, April

26, 1957. 5 p. 4 figs. DWB--Not only SID's but gradual

ionospheric disturbances (SWF) are associated with solar

flares in 79% of the cases and with GWF in 85% of the cases

(based on 69 selected dates). Sample records are presented

and analyzed. (Met. Abst. 9. 8-157. )--M. R.

D-458 Lindquist, Rune, Ionospheric effects of solar flares: preliminary reports Nos. 2 and 3. GSteborg, Sweden, Chalmers

Tekniska HSgskola, Handlingar, No. 95, 1950. 11 p. diagrs.,

tables. Reports from the Research Laboratory of Electronics,

No. 13. DWB--Results of fadeout recordings made at the Ionospheric and Radio wave Propagation Observatories at Gothenburg, Sweden from July 1948-June 1949 are presented in tables

and graphs. (Met. Abst. 7. 10-306. )--M. R.

D-459 Lindquist, R. (Ionospheric Res. Lab., Pa. St. Coll.), An

investigation of the ionizing effect in the E layer near sunrise. Journal of Geophysical Research, 57(4):439-458, Dec. 1952.

9 figs., 31 eqs. MH-BH. Also: Pennsylvania. State College.

Ionospheric Research Laboratory, Contract AF 19(122)-44,

Scientific Report, No. 34, March 20, 1952. 59 p. 18 figs.

,

41 tables, 20 refs. , 38 eqs. DWB--This paper discusses the

pre -sunrise decrease in height of the reflection point noted in

150 kc/sec vertical incidence group height recordings. It is

shown that the local time of this decrease has a pronounced

seasonal variation. The total number of particles along the

sun ray to the reflection point where the height decrease begins has been computed. This number is almost constant

throughout the year, yielding a value of about 3. 3 X 10^0 atmospheric particles. By considering the composition of the

upper atmosphere, it is shown that the only constituent which

might possibly be subject to the pre-sunrise ionization is Oo.

The corresponding solar radiation should have A >• 910 A,

The value for the absorption coefficient of O2 obtained from

162
+ -19 2

these considerations is K02 = (3. 3 — 2. 1) X 10 cm . It is shown that the pre-sunrise ionization is not due to a pure

screening effect. (Met. Abst. 4. 9-255. )--Author's abstract.

D-460 Little, C.Gordon, A diffraction theory of the scintillation of

stars on optical and radio wavelengths. Royal Astronomical

Society, Monthly Notices, 3(3):289-302, 1951. 3 figs. , 2

tables, 20 refs., eqs. DWB--Author makes 3 objections to

refraction theory of scintillation and then sets out theory of

Fresnel diffraction in a nonhomogeneous disturbing layer.

This corresponds with that of BOOKER, RATCLIFFE and

SCHINN for radio waves. The path change requires density

gradients of 0. 003% in 5 cm (i. e. a temperature gradient of

0. 002 C/cm for refraction theory) in a disturbing layer C. 2

km thick. The effect varies with wavelength and gives color

changes. Theory is applied to local fluctuations of radio

wave lengths from stars, caused by irregularities of about

5 km in F2 layer travelling at about 1000 km/hr. (Met. Abst.

3.9-227.)«C.E.P.B.

D-461 Little, C.G. and Maxwell, A. (both, Jodrell Bank Exp. Sta.

,

Manchester Univ. ), Fluctuations in the intensity of radio

waves from galactic sources. Philosophical Magazine, A,

42:267-278, 1951: 5 figs., 2 tables, 9 refs. DLC --Describes

experiments conducted (May 1949-Dec. 1950) with the purpose

of investigating (1) the correlation between fluctuations and

local ionospheric phenomena; (2) changes in amplitude and

period of fluctuations with elevation of source; and (3) to determine the linear dimensions of ionospheric irregularities re- sponsible for the fluctuations. The observations of Cygnus

and Cassiopeia, taken over a wide range of angles of elevation, are discussed along with the spaced receiver observations over 0. 1, 4, and 11 km base lines enabling determination of the scale of radio energy diffraction pattern across the

ground. --W. N.

D-462 Little, C.G. , The origin of the fluctuations in galactic radio

noise. Ph. D. Thesis, Univ. of Manchester, 1952. (unchecked)

D-463 Little, C.G. and Maxwell, A., Scintillation of radio stars

during aurorae and magnetic storms. Journal of Atmospheric

and Terrestrial Physics, London, 2(6):356-360, 1952. 3 figs.,

6 refs. DWB—Scintillations of radio stars on 3. 7 m during

auroras of Sept. 25 and Oct. 28, 1951, averaged 4 or more

per minute compared with 1-2 in normal conditions. On Oct.

28 a 10% decrease of signal intensity at maximum aurora occurred. Scintillation rate also has high + correlation with

geomagnetic K index. Records of receivers 3 km apart show

that changes of fluctuation rate are due to changes in speed

163
of passage of quasi-stable disturbances, which may be about

120 km across. During aurora, average wind speed in upper

ionosphere was about 400 m/sec; changes in scintillation

rate are due to changes in this velocity. (Met. Abst. 5C207J--C.E.P.B.

D-464 Little, C.G. , High latitude ionospheric observations using

extraterrestrial radio waves. Institute of Radio Engineers,

N.Y. , Proceedings, 42(11):1700-1701, Nov. 1954. 4 figs.

,

4 refs. Ibid: URSI Information Bulletin, No. 94:36-41, Nov. - Dec. 1955. --Describes method and discusses the results of

observations of ionospheric effects on extraterrestrial incoming radio waves at College, Alaska, during March 16-May

1954. Absorption at 65 Mc/s was stronger around midday,

was correlated with polar blackouts and found to be linked

to the variability of earth's magnetic field. Findings indicative of nonuniform lateral distribution of ionization are considered. --W. N.

D-465 Little, C.G. ; Rayton, W. M. and Roof, R.B. , Ionospheric

effects at VHF and UHF. Alaska Univ. Geophysical Institute

Contract AF 39(635) -2887, Technical Report No. 1, Oct. 1955.

104 p. 8 sections, numerous refs. DWB--The report consists

of sections summarizing knowledge of radar reflections from

aurora, absorption, radio noise of auroral origin, refraction

of radio waves by the ionosphere, the scintillation of radio

stars, radar echoes from moon, and radar echoes from meteors

Each of these is in turn divided into subtopics and particular

emphasis is given to references to original papers and concerned agencies. (Met. Abst. unpub. )--E. Z. S.

D-466 Little, C. G. ; Rayton, W. M. and Roof, R. G. , Review of

ionospheric effects at VHF and UHF. Institute of Radio Engineers, N. Y. , Proceedings, 44(8):992-1018, Aug. 1956.

2 tables, 182 refs. , 3+ eqs. DLC--This paper summarizes

the present day knowledge of ionospheric effects at VHF and

UHF, with the exception of forward scattering of VHF radio

waves by the ionosphere. The seven effects covered in the

paper are: Radar echoes from aurora, radar echoes from meteors, the Faraday effect and radar echoes from the moon,

radio noise of auroral origin, absorption of radio waves by

the ionosphere, refraction of radio waves by the ionosphere,

and the scintillation of the radio stars. Each ionospheric

effect has in turn been divided into separate subtopics, and

the main results are given in these sub-sections, with particular emphasis upon providing references to the original

papers. In this way the reader wishing to know the answer

to a specific problem will speedily be able to find a summary

of the main published results in the field, and also be able to

learn which papers deal with the particular topic of interest.

(Met. Abst. 8H-81. )--Authors' abstract.

164
D-467 Little, C.G., Radio astronomy as a tool for studying the

ionosphere at VHF. Conference on Arctic Radio Wave Propagation, Alaska Univ. , Jan. 1956, Papers, Issued May 1956.

p. 2-7. (Unchecked)

D-468 Little, C.G. ; Merritt, Robert P. ; Rumi, G.C. ; Stiltner,

Ernest and Cognard, Rene, Radio properties of the auroral

ionosphere. Alaska. Univ. Geophysical Institute, Contract

AF 30(635) -2887, Quarterly Progress Reports, No. 1-5, 7,8,

June 1, 1956-May 31, 1958. 1 piece (53 p. ) 16 figs. , 13

tables, lOrefs., numerous eqs. DWB (M94. 6 A323ra)--This

report describes the results of more than twelve months operation of the 223 Mc and 456 Mc phase switch interferometers.

The magnitude of the 223 Mc amplitude and angular scintillations effects have been determined at an auroral latitude using

two extraterrestrial radio sources. These magnitudes are discussed in terms probability distributions, mean values, and

diurnal, azimuthal, elevations, and source effects, a) The

probability of occurrence of each of the five main levels of

223 Mc scintillation activity is given; b) Typical amplitude

probability distributions and mean values of tractional deviation in power are given for each of these indexes; c) Representative values of mean angular scintillation, and probability distribution for angular scintillation are given for each

main 223 Mc scintillation index; d) The diurnal variation for

both sources shows a maximum of scintillation activity at

about magnetic midnight ( /"-v-'0140 AST), with a ratio of about

1.8 to 1 between maximum and minimum. It is suggested that

the activity is controlled in part by magnetic time; e) An azimuthal dependence has been found for the Cygnus source,

which scintillates most strongly when seen toward magnetic

north (some 30 degrees east of true north). It is suggested

that the activity is controlled in part by the magnetic latitude

at which the ionosphere is traversed; f) Both sources show

very little variation of scintillation activity with zenith angle.

(Cygnus covers the range 24 degrees zenith distance to 75

degrees, Cassiopeia 6 degrees to 57 degrees.) This lack of

zenith angle dependence is attributed to the elongation of the

irregularities along the earth's magnetic lines of force; g)

The scintillation activities of the two sources are different.

These differences are attributed to the larger subtension of

the Cassiopeia source; h) A recent paper on the theory of

radio star scintillations is modified to take into account an

elongation of the ionospheric irregularities along the magnetic

field lines. Note that the occurrence of radio star fades, as

observed on phase switch and phase sweep interferometers,

has already been reported and described in Quarterly Progress

Report No. 6. (Met. Abst. 11E-89. )--Authors' abstract.

165
D-469 Little, C.G. and Leinbach, H. , Some measurements of high

latitude ionospheric absorption using extraterrestrial radio

waves. Institute of Radio Engineers, N. Y. , Proceedings,

46(1): 334-348, Jan. 1958. 21 figs. , 2 tables, eqs. DLC.

Separated pages issued as Alaska. Univ. Geophysical Institute, Contributions, Ser. B, No. 22, 1958. DWB--Outline of

the ionospheric absorption theory is given along with description of instrumentation and methods of measurement. With

the objectives of checking the geographical extent of the absorbing "clouds" diurnal variation, height of absorbing re- gion, correlation between magnetic activity and absorption,

and correlation between aurora and absorption, three different

experiments with 30 Mc extraterrestrial waves were conducted:

1) with rotating antenna, March 1955 at College, Alaska; 2)

with two antennas, summer 1956; and 3) over a distance of

800 km between College and Barrow, Alaska, spring 1957.

The results discussed are presented in graphs and tables.

Findings were: Absorption was greatest in northern quadrant

and extended well over 100 km, and at least 800 Km during

disturbances. All absorption occurs below E region at about

60 Km. Pulsating and flaming auroras alone are intimately

associated with major absorption, suggesting quite a different

physical mechanism from other auroras. (Met. Abst. 11E-90)

--W. N.

D-470 Little, C. G. and Leinbach, H. , The riometer — a device for

the continuous measurement of ionospheric absorption. Institute of Radio Engineers, N. Y. , Proceedings, 47(2):315-320,

Feb. 1959. 4 figs., 6 refs. DLC--A sensitive, self-balancing, noise measuring equipment, known as the riometer, is

described. This instrument has been designed for routine mea

surement of ionospheric absorption during the IGY, using the

cosmic noise method. Application of this technique in the

auroral zone has resulted in quantitative measurements of ionospheric absorption, even during polar blackouts. The riometer has the advantages over a simple total power cosmic

noise receiving system of 1) linear response to changes of input noise power, 2) high accuracy in the presence of narrow

band RF interference, and 3) good long term stability. (Met.

Abst. 1 IE -91. ) -Authors' abstract.

D-471 Little, C.G. and Lawrence, Roberts., The use of polarization fading of satellite signals to study the electron content

and irregularities in the ionosphere. U. S. National Bureau of

Standards, Journal of Research, Sec. D, 64(4): 335-346, July/

Aug. 1960. 11 figs. , 15 refs. , 4 eqs. DWB, DLC--A procedure is described for using the Faraday rotation fading of a

satellite radio signal to measure the ionospheric electron content per unit column up to the height of the satellite. At frequencies as low as 20 Mc the rotation of the plane of

166
polarization cannot be assumed to be proportional to ^>NB

cos Q d along the line of sight. The simplifying assumptions implied by this expression are avoided, and full ac- count is taken of ionospheric refraction, using the collisionfree form of the Appleton-Hartree equation. Results based

on observations of 1958 Delta 2 are presented. The subsatellite electron contents have been derived throughout the satellite passes for heights both above and below the F peak,

the latter compare well with values derived from simultaneous

ionograms. The method also permits the study of large scale

irregularities in electron content. Such irregularities, having

lateral dimensions of a few hundred kilometers and fractional

deviations in subsatellite electron content of about 0. 01, have

been detected. Our observations suggest that satellite polarization studies offer important advantages over other methods

of investigating these irregularities. (Met. Abst. 11. 11-54

--Authors' abstract.

D-472 Liszka, Ludwik (Kiruna Geophys. Obs. , Sweden), A type

of variation of the signal strength from 1958 %2 (Sputnik 3) . Nature, London, 183(4672): 1383- 1384, May 16, 1959. 3 figs.,

ref. DWB--The results of some 200 passings of Sputnik 3, as

observed at Kiruna Geophysical Observatory (67.8 N, 20.4 E),

Sweden, by means of the 20. 005 Mc/s radio signals, seemed

to fall into pattern linked to definite points of the satellite's

orbit. Hence, the purpose of this paper is to test the hypothesis whether the satellite produced heavily ionized tracks of

relatively long existence. The initial study is by calculating

the mean weight w of 85 night passages for which the results are plotted. The study is to be continued. (Met. Abst. un- pub. )-W. N.

D-473 Liszka, L. (Kiruna Geophys. Obs. , Sweden), Dropout phenomenon observed in the satellite 1958 o2 transmissions.

Journal of Geophysical Research, Wash., D.C., 66(5):1573-

1577, May 1961. 6 figs. , 5 refs. DLC --During the period

between March 1959 and April 1960, when the amplitude of

1958 & 2 transmissions were measured at Kiruna Geophysical

Observatory, sudden decreases of observed signal strength,

usually to the noise level, were occasionally recorded. Synchronous amplitude measurements at several European stations showed that the phenomena coincided exactly. The fall

in amplitude was invariably accompanied by a rapid decrease

of observed frequency by up to 50 cps/s. At the termination

of dropout, the frequency returned to the regular Doppler

curve, and the subsequent rate of change was usually lower

than at the onset. Similar dropout effects were observed on

transmission of Explorer VII at 19. 9904 Mc/s. The author

rejects two explanations of this dropout and proposes that

the data from Kiruna supports the hypothesis that the

167
phenomenon is an effect of radiation on the satellite transmitter. The radiation probably from secondary Trays produced by high energy electrons in the upper atmosphere or

in the satellite itself, is manifested during period of giant

magnetic pulsations when the satellite passes through sufficiently dense regions of the lower horn of the outer Van

Allen belt. (Met. Abst. unpub. )--From author's text.

D-474 Lodge, Sir Oliver Joseph, Signalling across space without

wires. Being a description of the work of Hertz and his suc- cessors, with additional remarks concerning the application

to telegraphy, and later developments. 3rd. ed. London,

The Electrician Printing and Publishing Co. , 1900. 133 p.

67 figs. --The first 42 pages contain notes and material used

in the lecture which author delivered before the Royal Institution of Great Britain, June 1, 1884. Several original, as

well as control experiments conducted by the author are included. Of historic interest is the first vague attempt to

measure radio wave emission from the galaxy. Seen in re- lation to its time, the lecture was a source of inspiration

to contemporary research workers. For example, "telegraphic

application based upon information given in the preceding lecture was made in 1895 by Professor Popoff. . . ". --W. N.

D-475 Lovell, A. C.B. and CIegg, J. A. , Radio astronomy, London,

Chapman and Hall, 1952. 238 p. 120 figs. , 7 tables, refs.

Frontiers of Science Series. Also transl. into Russian by

B. M. Chikhachev as Radioastronomiia. Moscow, Izdat.

Inostrannoi Literatury, 1953. 240 p. 120 figs. , 7 tables,

numerous foot -refs. , eqs. Refs. at end of most chapters.

DLC--After introductory chapters on astronomy and the transmission and reception of electromagnetic waves, this popular

book takes up the study of meteors by radio echo, its results

and significance, radio waves from the sun, sunspots and

solar flares, radio waves from the galaxy, twinkling of radio

stars, the aurora, radio investigation of the moon and the

planets, and afterglow. The translation includes critical comments; references are given in original form but with Russian

references added or substituted in several chapters; illustrations are well reproduced. (Met. Abst. 9A-20. )--C. E.P. B.

,

M.R.

D-476 Lovell, A. C.B. , Report on Jodrell Bank to the Royal Astronomical Society Council for 1951. Royal Astronomical Society,

Monthly Notice, 112( ):302-305. --A brief report summarizing

the work being carried out at Jodrell Bank. Discusses radio

frequency emissions from extra-galactic nebulae; from the galaxy; scintillations of radio stars; solar radio frequency emissions; the velocity distributions of sporadic meteors; the daytime meteor streams; the night-time meteor streams; the

168
continuous meteor survey; meteor heights; scattering of radio

waves from meteor trails; behavior of meteor trails after formation; radio echoes from the Aurora Borealis and from the

moon. --L. A. Manning.

D-477 Lovell, A.C.B. , Radio astronomy and the fringe of the atmos - phere. Royal Meteorological Society, Quarterly Journal,

82(351):1-14, Jan. 1956. 13 figs. , 54 refs. DWB--This

Symons Memorial Lecture summarizes 6 branches of radio as- tronomy. Scintillation of radio stars is due to elongated ionized clouds in the F region about 400 km moving with an aver- age speed of 100 m/s in 50-60 N to 360 m/s in the auroral zone. The apparent predominance of E-W and W-E motion may

be due to the shape of the clouds. Drifts of radar reflections

from ionized meteor trails at 70-120 km have given much information about semidiurnal and annual variation of winds. Scale

heights, pressures and diffusion coefficients in the 100 km

region can also be determined by radio echo meteor techniques. Sec. 6 describes the investigation of auroras by radio

echoes, including determination of drift velocities (which are probably not due to winds). Finally, the bearing of moon

echoes on the total electron content of the ionosphere is mentioned. (Met. Abst. 12E-96. )--C.E.P.B.

D-478 Lovell, A.C.B. (Jodrell Bank Experimental Station), Radio

astronomical measurements from earth satellites. Royal Society of London, Proceedings, Ser. A, 253(1275):494-500, Dec.

29, 1959. 3 figs., 16 refs. DWB, DLC -It may be thought

that radio astronomical measurements made on the earth are not subject to the influence of the atmosphere and ionosphere

to any great extent and that consequently there is no demand

for measurements from earth satellites or other space stations.

Unfortunately, this is not the case and certain measurements

from outside the earth's atmosphere are very much desired.

The radio spectrum so far explored extends from a low frequency limit in the 10 to 20 Mc/s band, to an upper limit in the

millimeter waveband. In the millimeter band the limitation to

the extension of the spectrum arises from absorption bands in

the atmosphere, whereas at low frequencies the extension is

limited by absorption and disturbances in the ionosphere. In

this paper some examples are given of the need to overcome

these obstacles. (Met. Abst. 11. 12-39. )--Author's abstract.

D-479 Lovell, A.C.B. (Jodrell Bank Experimental Station, Univ. of

Manchester), The exploration of outer space. Observatory,

London, 80(915) :64-72, April 1960. DLC (QB1 02)-A review

is given of what is known about the Van Allen radiation belts.

It is suggested that similar radiation belts may surround the

other planets of the solar system. No such belts have been

found near the moon but this is not unexpected. The outer

169
radiation belt is obviously linked with the major geophysical

effect observed on the earth and seems to act as a reservoir

of charged particles with the sun as a source and the earth as

a sink. Radio observations of the sun show the sun to be of

varying size according to the wave length used. It seems

probable that there is a constant outward streaming of particulate material from the sun. This gives rise to what is termed

the solar wind which appears to envelop the planets. More

detailed studies of the moon and planets are projected using

both satellite and radiotelescope techniques. An account is

given of the results which it is hoped to achieve. The article

concludes with a description of what is known about general

cosmology and the possibilities of radio astronomy. (Met.

Abst. 12. 4-159. )--R.B.

D-480 Low, Ward C. and Knight, Raymond M. , Rocket reception

of radio pulses over long distances. Boston University.

Upper Atmosphere Research Laboratory/ Contract AF 19(122)-

36, Investigation of the ionosphere utilizing sounding rockets.

Final Report, June 30, 1953. 65 p. tables, numerous figs.

MH-BH--This is the final report on Contract AF 19(122)-36 between the Dept. of Defense and the Trustees of Boston Univ.

It also marks the conclusion of the project usually termed the

"Oblique Incidence Ionosphere Experiment/' here called briefly the "Ionosphere Experiment." The principal goal of this

project has been to obtain general information concerning

characteristics of long distance radio pulse reception in high

altitude rockets, more specifically, whether significant deviations from results of simple propagation theory result from the

receiving stations being in, or very near, the E layer. To the

limited extent to which the recovered data have been examined

no such anomalies have been recognized. A description of the

equipment employed on this experiment in three high altitude

missiles: V-2 No. 51, and AFCRC Aerobee Rounds No. 20

and No. 24 is presented. A display of data obtained during

the flights of those missiles is given, with a discussion of

the methods of measurement used. (Met. Abst. 5. 7-41. )--

Authors' abstract.

D-481 Ludwig, George H. and Whelpley, William A. (both, State

Univ. of Iowa), Corpuscular radiation experiment of satellite

1959 Iota (Explorer VII) . Journal of Geophysical Research,

Wash. , D. C. , 65(4): 1119-1124, April 1960. 6 figs. , 5 tables.

DLC --Satellite 1959 Iota (Explorer VII) carries an apparatus

prepared by the Dept. of Physics and Astronomy of the State

Univ. of Iowa for comprehensive spatial and temporal monitoring of total cosmic ray intensity, geomagnetically trapped cor puscular radiation, and solar protons. In view of the successful operation of the equipment during the first 2 months of

flight and the expectation of its continued operation until

170
Oct. I960, we have considered it desirable and worth while

to invite international participation in the recording and interpretation of the radiation observations. A full description

of the apparatus is given, including detector calibrations,

telemetry code, samples of actual recordings, and other pertinent information. (Met. Abst. 11. 12-594. ) -Authors' abstract.

D-482 Lugeon, Jean, L 'eclipse de soleil du 31 aout 1932 et le sondage par les parasites atmospherigues. (Solar eclipse of Aug.

31, 1932, and soundings by means of atmospheric parasites.

)

Academie des Sciences, Paris, Comptes Rendus, 195:817-

819, Nov. 7, 1932. 3 figs. DLC--By comparing records from

sferics recorders installed by the author during the Polar Year

at Jablonna (near Warsaw), at Tromsjrf, Norway and on Bear

Island during the eclipse of Aug. 31, 1932, it is established

in both a positive and a negative manner that the grazing rays

of the sun just striking the ionosphere mark the time of ending

or beginning of strong sferics reception from sources thousands

of miles distant. The sources in this case were from the U.S.

A. and they were clearly received during eclipse only at JabKonna which lay in right geometric path for the eclipse influence to be felt, but not at the Norwegian or Bear Island stations. The eclipse effect is similar to sunset effect. (Met.

Abst. 4K-91.)-M.R.

D-483 MacArthur, J. W. (Marlboro College, Marlboro, Vermont),

Theory of the origin of the very low frequency radio emissions

from the earth's exosphere. Physical Review Letters, N. Y.

,

2(12):491-492, June 15, 1959. 2 refs. , 7 eqs. DWB, DLC--

A Doppler and proton-gyro concept is shown to be complementary rather than exclusive to (Gallet's) traveling wave tube

mechanism, hence work in progress may explain all types of

dawn chorus by this combination process. (Met. Abst. 11. 9-

108.)»W.N.

D-484 McCoy, D. O. , An all-weather radio sextant. Navigation,

Los Angeles, 4(8):309-319, Dec. 1955. DWB, DLC--The automatic sun tracking sextant (of which three types are described

and illustrated along with modus operandi outlined in simple

diagram) is mainly characterized by its immunity to weather

for accurate performance. Data obtained at 1. 9 cm and 8. 7

mm wave lengths are discussed briefly since more complete

results are to be published from the experiments at Feather

Ridge Observatory. Results from such experiments (1952

cases) at 8. 7 mm wave length is given in a curve showing

only 0. 017 probable error of integral distribution for altitudes

above 30 . Lunar tracking has been done experimentally, with

better results than were obtained from radio stars strong enough

for tracking with the radio sextant. (Met. Abst. 9B-124)--W. N.

171
D-485 Mcintosh, Douglas Haig, Geomagnetic solar flare effects at

Lerwick and Eskdalemuir. and relationship with allied ionospheric effects . Journal of Atmospheric and Terrestrial Physics,

1(5/6) :315-342, 1951. 3 figs., 22 tables, 19 refs. DWB--

The geomagnetic effects of solar flares (the crochets) over the

period 1936-1949 are tabulated and identified. An equinoctial

maximum of occurrence is observed. Midday is the hour of

greatest frequency. The relationships between geomagnetic

effects and flares, fade outs, sudden enhancements of sferics,

etc. , are examined. A general discussion of the phenomena

is given. (Met. Abst. 4. 3-105. )--A. A.

D-486 McKerrow, C.A. , Sudden decrease in low frequency atmospheric noise during the cosmic radiation storm of Feb. 23. Nature, London, 177(4522):1223-1224, June 30, 1956. fig.

DWB--At Churchill, Manitoba, a sudden decrease of 100 kc/s

noise occurred at 0345 G. m. t. Other observations are compared and it is concluded that u for this solar flare there appeared to be a sudden increase in the D region absorption on

the darkened half of the hemisphere which cannot be attributed

to ultraviolet radiation. It also appears that this condition

may occur only at high latitudes situated near the auroral zone

(Met. Abst. 7. 10-175. )--C.E.P.B.

D-487 McLean, D. J. (School of Physics, Univ. Sydney), Solar

radio emission of spectral type IV and its association with

geomagnetic storms . Australian Journal of Physics, Melbourne,

12(4):404-417, Dec. 1959. 5 figs. , 2 tables, 14 refs. DLCA new type of solar radio event, the type IV storm, first described by BOISCHOT, has been identified on Dapto radio spectographic records. It has been shown to be distinguishable

from type I storms by 1) its smooth spectrum, 2) its close as- sociation with type II bursts, and 3) its remarkably close as- sociation with geomagnetic storms. In common with some type

I storms, all type IV storms are found to be associated with

very large solar flares. It appears possible to explain the production of type IV emission and the occurrence of the related

phenomena in terms of a single cloud of gas which moves

through the Sun's corona. (Met. Abst. 11. 10-201. )--Author's

abstract.

D-488 Magnuson, G. D. and Medved, D. B. (both, Physics Section

of Convair, San Diego, Calif. ), Sputtering as a possible

mechanism for increase of ionization in the vicinity of low

altitude satellites. Planetary and Space Science, 5(2):115-

121, June 1961. 3 figs. , 2 tables, 4 refs. , 17 eqs. DLC--

It is suggested that for altitudes below 200 km there may be

sufficient sputtering produced by ion, atomic, and molecular

impact on the vehicle surface to lead to some increase in

ionization above ambient at distances of one mean path or

172
less from the vehicle. The sputtering process injects into

the environment atoms of metallic elements whose ionization

potentials are 1/2 to 1/3 those of the ambient species. Collision energies in the center of mass system vary from ionization thresholds (Ej) to 2 to 3 times Ej. The resulting ionization in the surroundings may then be calculated if values

for fi t the probability of any collision leading to ionization

is known. On the basis of the crude model presented, /9

should be greater than, or equal to, 10"° for this mechanism

to be of interest. (Met. Abst. unpub. )--Authors' abstract.

D-489 Malik, Chester; Aarons, Jules and Poeverlein, Hermann

(all, A. F.Cambridge Res. Center, Bedford, Mass.), Backscatter experiments during the total eclipse of Oct. 2, 1959.

Journal of Geophysical Research, Wash. , D. C. , 65(10):3241 - 3247, Oct. 1960. 5 figs. , 7 refs. DLC -Backscatter records

taken at 19. 39 Mc/s with a rotating antenna were investigated in order to determine how the returns were affected by the

total eclipse of Oct. 2, 1959. At the frequency chosen,

ground backscatter via F layer reflection sets in before sunrise at the location of observation. On normal days before

and after the eclipse, it appears first in the east and southeast and then, 2 or 3 hours later, in the west. On the eclipse

day, the signal from the east was delayed several hours and

appeared after the return from the west had been received.

Graphical representations of details of the backscatter re- cords show not only the eclipse effect but also the effect of

ionospheric disturbances on days before and after the eclipse.

These disturbances make it nearly impossible to formulate a standard of average behavior that may be quantitatively compared with the eclipse day. The long duration of the eclipse

effect indicates its complicated nature which probably involves dynamic properties of the F2 layer. (Met. Abst. 11L315. ) --Authors' abstract.

D-490 Malinge, Anne-Marie (Observatoire de Meudon), Relation

entre les orages radioelectriques solaires et les eruptions

chromospherigues

(Relationship between solar radio noise

storms and solar flares. ) Annates d'Astrophysique, Paris,

23(4): 574-584, July/Aug. 1960. 5 figs. , 8 refs. French,

English and Russian summaries p. 574. DWB, DLC--Comparisom of the position of radio noise storms observed at 169 MHz

with solar flares following or preceding the beginning of the

noise storms shows a definite relation between the two phenomena. A notable effect of refraction is shown to exist in the corona. (Met. Abst. 11L-99. )--Author's abstract.

173
D-491 Malurkar, S.L., The solar flare effect at Alibaq on June 13.

1951 . Annali di Geofisica, 7(2):215-219f April 1954. fig.,

3 tables. DLC--A detailed study of the quick-run magnetograms of the solar flare of June 13, 1951. Alibag was favorably situated. Corresponding to different flares on that day

the profile of the solar flare effect has two stage maximum.

The time of the onset of the radio fadeout in relation to the

flare has been pointed out. In the vertical force effect cor- responding to the onset and end of radio fadeout there has

been a temporary no-variation-with -time stage or a sort of

inflexion. The diurnal range of ozone at Troms/rf also was abnormally large within the next 24 hours. (Met. Abst. 9B-96.

)

--Author's abstract.

D-492 Mandel'shtam, S.L. and Efremov, A. I. , Issledovaniia korot- kovolnovoqo ultrafioletovoqo izlucheniia solntsa. (Investigation of short wave ultraviolet solar radiation. ) Uspekhi Fizicheskikh Nauk, Moscow, 63(1): 163-180, Sept. 1957. 13 figs.,

5 tables, 24 refs. DLC. Transl. available LC or SLA. mi

$2. 70 phot. $4. 80. —The present paper sets out briefly the

results of experimental and theoretical work on the study of

the short wave emission from the sun published since an earlier review (Ibid. , 1952). Experiments are also described

which, it is suggested, could be profitably carried out with

the aid of an artificial earth satellite. (Met. Abst. 11J-103.

)

--Physics Abstracts * D-493 Marini, J. W. (Electromagnetic Res. Corp., Wash. , D. C),

Radiation and admittance of a slotted sphere antenna surround- ed by a plasma sheath. Planetary and Space Science, N. Y.

,

6:116-122, June 1961. 2 figs. , 3 refs. , 16 eqs. DWB--On

the simplified assumptions that the frequency is low and the

sheath strongly ionized, expressions for the input impedance

of the slot, the radiation pattern and the power loss are obtained. Criterion for thickness of the insulating layer that

conduction losses in the sheath be small is established. Input admittance and external efficiency of the antenna are determined. --W. N.

D-494 Marmo, F. F. ; Aschenbrand, L. M. and Pressman, J. (all,

Geophys. Res. Directorate. A. F., Cambridge Res. Center

L. G. Hanscom Field, Bedford, Mass.), Artificial electron

clouds. I. Summary report on the creation of artificial electron clouds in the upper atmosphere. Planetary and Space

Science, l(3):227-237, Aug. 1959. 3 figs. , 4 tables, 3 refs.

DLC --This is the first paper of a series dealing with the ex- perimental results of artificial electron clouds as produced at

70 and 130 km altitude for the study of the upper atmosphere.

A method of correlating optical and radio-radar data is included

174
in this general survey of methods and techniques. Tabulated

results from the first experiments, which began March 1956

at Holloman Air Force Base, New Mexico, are presented.

Other locations for experiments are in Texas, Colorado, Utah

and Arizona. --W. N.

D-495 Marner, Gene R. , Atmospheric attenuation of microwave

radiation. Institute of Radio Engineers, Professional Group

on Antennas and Propagation, Transactions, Vol. AP, 3(1):

68-71, 1955. DLC--A combined radio telescope - radio sextant was used to measure atmospheric attenuation at a wavelength of 8. 7 mm. --CSIRO Abstract.

D-496 Marner, G. R. (Collins Radio Co. ), Automatic radio-celestial navigation. Institute of Navigation, London, Journal,

12(3/4): 249-259, July/Oct. 1959. 6 figs. (incl. photos),

table, 13 refs. , 5 eqs. DWB, DLC —Describes the features

of the radio sextant and indicates the possibility of its use

for automatic navigation. Two radio sextants are described

and shown in photographs: 1) the experimental sextant completed in 1952 (Collins Radio Co. ) presently in use aboard

the U.S.S. "Arneb"; and 2) a radio sextant (MARNER and

WILLIS, 1959) capable of tracking both the sun and moon

with high precision. In the light of experiments with these

instruments the entire problem of radio-celestial navigation

is examined in minute detail. It is found that the use of the

discrete sources of radio radiation does not appear practical

with a small antenna due to the low flux density at microwave wavelengths and to competing atmospheric emission

effects. However, the automatic radio sextant has demonstrated its capability for precise solar and lunar tracking in

both clear and foul weather with an antenna of modest size.

(Met. Abst. 11.9-107. M.S.

D-497

D-498

Marshall, Alan C. and Houston, Robert E. , Ins trumentation

for the automatic Doppler tracking of earth satellite radio

signals. New Hampshire Univ. , Contract AF 19(604) -4145,

Scientific Report, No. 1, July 1961. 38 p. 9 figs., ref. -- Detailed description in text and block diagrams is given of a simple but reliable instrumentation used effectively since

1958 for automatic tracking of the Doppler shift of passing

satellites. Greatly extended usefulness of this prototype

instrument is feasible with slight modifications. A few re- cords of observations taken are included. (Met. Abst. un- pub. )--W. N.

Martyn, D. F. (Indust. Res. Organ., Camden, N. S. W. ), Sporadic E region ionization. 'Spread F', and the twinkling of

radio stars. Nature, London, 183(4672): 1382-1383, May 16,

1959. fig., 6 refs., 2 eqs. DWB--

175
An explanation of these phenomena is given„ It is shown

how the kinematically unstable surface ionization of the upward drifting F region and the simultaneous down-drift (or

rather lag) of small irregularities become capable of producing the pronounced scattering responsible for scintillation

and "spread F*. In the E region a cyclindrical perturbation

with travel through the medium as a wave which is almost

certain to be accountable for the equatorial sporadic E re- gion ionization. It is the kinematic instability in the ionization gradient of a medium drifting across a magnetic field

which basically governs the above phenomena. (Met. Abst.

11. 9-121. )-W.N.

D-499 Massachusetts Institute of Technology. Lincoln Laboratory,

Collection of Soviet papers on earth satellites. Issued Oct.

31, 1957; reissued Jan. 13, 1958. 182 p. figs. , tables,

refs., eqs. DWB (629. 1388 M414co) -Contents: Vakhnin,

V., Artificial earth satellites (from Radio, No. 6:14-17, June

1957). Kazantsev, A. N. , Observation of radio signals from

an artificial earth satellite and their scientific value, p. 6-

15 (from Radio, No. 6:17-19, June 1957). Makhailov, A. A.

,

Observation of the artificial satellite, p. 16 (from Astronomicheskii Tsirkuliar, No. 180:1, May 18, 1957). The following papers were all originally printed in Uspekhi Fizicheskikh

Nauk, Moscow, Vol. 63, No. 1, Sept. 1957. Danilin, B. Set al. , Problem of the measurement of pressure and density

of the upper layers of the atmosphere with the aid of an artificial earth satellite, p. 17-48. Ginzburg, V.L., Use of

artificial earth satellites for the purpose of proving general

relativity theory, p. 49-54. Mikhnevich, V. V. , Measurement of pressure in the upper atmosphere, p. 55-65. Vernov.

S. N. et al. , Investigation of the composition of primary cosmic rays, p. 66-88. Vavilov, V.S. et al. , Silicon solar batteries as electric power sources for artificial earth satellites,

p. 104-112. Iatsunskii, I. M. , The effect of geophysical

factors on satellite motion, p. 113-130. Okhotsimskii, D. E.

et al. , Determining the lifetime of an artificial earth satellite

and an investigation of secular perturbations of its orbit, p.

131-152. Poloskov, S. M. and Nazarova, T. N. , Investigation of solid components of interplanetary matter by means of

rockets and artificial earth satellites, p. 153-170. Taratynova, G. P. , Motion of an artificial satellite in the noncentral

gravitational field of the earth in the presence of atmospheric

resistance. (Met. Abst. 10. 10-4.

)

176
D-500 Massey, H. S. W. , The nature of the upper atmosphere. Endeavour, London, 13(50):81-85, April 1954. 4 figs. , 6 refs.

DLC --General but semitechnical treatment of structure and

composition of the high atmosphere, the ionosphere, aurora and airglow according to latest results of rocket and radio

research. (Met. Abst. 12E-70. )--M. R.

D-501 Massey, H.S. W. , Rockets and satellites in scientific re- search. Endeavour, London, 17(66) :85-89, April 1958. 2

refs., 4 eqs. DLC --Usefulness of rockets in obtaining ionospheric and high atmospheric composition, temperature, density, ionization and radiation data; limitations in time aloft

which are overcome by use of satellites, a history of sounding rockets, their instrumentation and future prospects, the

orbits and some of the results of the first U. S. and Soviet

satellites are reviewed for general information. The results

of ejection of sodium vapor and of NO at high altitudes (40-

60 mi) are also discussed. The fluorescence from the sodium

vapor cloud persisted for 20 min, even at points 300 mi away

from the launching site. (Met. Abst. 10. 6-85. )--M. R.

D-502 Massey, H. S.W. and Boyd, R.L. F. , The upper atmosphere.

London, Hutchinson and Co. , 1958. 333 p. 12 figs., 21

plates, 6 tables, 20 refs. , 33 eqs. Price: 63 sh. DLC

(QC879. M3). Review by D. R. Bates in Nature, 182(4650):

1629, Dec. 13, 1959. --This is the latest and most systematic

book summarizing the current knowledge of the upper atmosphere (from 10 mi to several hundred mi above the surface) as

gained by study of geomagnetic fields, radio wave propagation, spectra, radiations; by means of balloons, rockets,

explosive waves, radio, spectroscopes, magnetometers, meteor photographs and spectra, cosmic ray counters or chambers, artificial satellites and other direct and indirect methods. Upper air temperature, composition, density; ionization, cosmic radiation (UV, visible, cosmic ray and radio

frequency), magnetic fields and electric currents, auroral and

airglow phenomena, ozone changes, twilight flashes and

glows, atmospheric tides, solar corpuscular streams and

other elements observed are tabulated. (Met. Abst. 10. 8-6.

)

~M. R.

D-503 Massey, H. S. W. and Boyd, R. L. F. , Scientific observations

of the artificial earth satellites and their analysis. Nature,

London, 181(4602): 78-80, Jan. 11, 1958. eqs. DWB--The

launching of the Soviet earth satellites took other governments by surprise. They were launched when tracking instruments in other parts of the world were inadequate and unsatisfactory. A list of the British stations engaged in the tracking

is given. The shortcomings and the achievements of the first

two satellites are included here. The potentialities of radar

177
method, the clear need for accurate orbit data, the computational procedures at the Smithsonian Institution and the need

to use the Faraday effect for determining ionospheric density

are also discussed. (Met. Abst. 10. 6-84. )--N. N.

D-504 Massey, H.S. W. (Dept. of Physics, Univ. College, London),

Scientific applications of rockets and satellites. (In: Symposium on High Altitude and Satellite Rockets, Cranfield, England, July 1957, (Proceedings). N. Y. , Philosophical Library,

1959. p. 7-14). DWB (629. 1388 S989hi)--Some of the more

important aspects of nigh altitude research by way of rocket

and satellite borne instruments are considered here. The topics include: studies of the solar spectrum before reaching the

earth's atmosphere, ionospheric refractive index, electron

concentration, the positive and negative ions, the dynamo

currents responsible for the quiet magnetic variations, the

soft x-radiation, airglow, production of ionized and metallic

clouds in relation to distribution of winds and temperature as

well as the basic properties of the atmosphere. The instrumentation comprises spectrographs with photographic recordings, photoelectric telemetering, photon counters, ion analyzers, magnetometers, photometers, etc. (Met. Abst. 111-

166. )-W. N.

D-505 Massey, H. S. W. (Chairman, British National Committee on

Space Research), Space research. Contemporary Physics,

London, l(2):81-95, Dec. 1959.-- Space research is defined

as the scientific study of the earth and the universe generally

which may be carried out using instruments conveyed by the

use of rocket motors to regions inaccessible in any other way.

This is a review paper of such research. The technical problems involve: 1. the rocket motor; 2. a guidance mechanism;

3. precise tracking techniques; 4. the development of suitable measuring instruments; 5. power supply for instruments;

6. relaying observation back to earth. Investigations which

may be carried out include: 1. study of the high atmosphere;

2. meteorological studies; 3. gravitational and magnetic

studies; 4. astronomical observations; 5. particle radiations in interplanetary space; 6. study of the nature of any

matter in interplanetary space; 7. study of the moon and

planets in situ; 8. investigation of the nature of gravitation.

(Met. Abst. 12. 4-53. )--R.B.

D-506 Matsushita, Sadami (Geophys. Inst. , Kyoto Univ. ), Semidiurnal lunar variations in the sporadic E. Journal of Geomagnetism and Geoelectricity, Kyoto, 4(l):39-40, April 1952.

2 figs. , 6 refs. DLC--An analysis of the critical frequency of

the sporadic E (fEs ) during summer solstice at Kokubunji,

Japan, lat. 139°29. 3'E, long. 35°42.2'N, for 1949-51 shows

the semidiurnal lunar variations in Es . Harmonic analysis of

178
these variations (shown in graph) gives an accurate picture

of the significant variations. It shows that on the average

the lunar semidiurnal variation reaches its maximum amplitude of 35 Mc/s or 13% about 8 hrs after the lunar culminations. The diurnal variations are usually of smaller amplitude than the semidiurnal. It was not possible to study the

variation in the Dec. solstice and the equinoxes because of

the small number of occurrences of Es . The amplitude of the

Es tide is greater than that in the E or F2. (Met. Abst. 9. 5-

137. )-M. R.

D-507 Matsushita, S. , Sequential Eg and lunar effects on the equatorial Es . Journal of Geomagnetism and Geoelectricity, Kyoto,

Japan, 7(3): 91 -95, Sept. 1955. 4 figs., 10 refs. DLC -Sequential Es is a type of sporadic E layer ionization which shows apparent vertical movement. Distribution of this phenomenon in

space and time is analyzed from world wide ionospheric data.

Lunar effects on Es and sequential Es are shown. (Met. Abst.

11D-95.)»G.T.

D-508 Matsushita, S. , Lunar effects on the equatorial Es. Journal

of Atmospheric and Terrestrial Physics, 10(3): 163-165, March

1957. 3 figs., 7 refs. DWB--Equatorial Es at Huancayo oc- casionally disappears suddenly near noon or early afternoon.

Local time of disappearance is earlier near full and new moon,

i. enduring first half of periods of westward lunar electric current. (Met. Abst. 8. 7-158. )--C.E.P.B.

D-509 Matthews, Whitney and Ludwig, George H. , Satellite telemetry. American Geophysical Union, Transactions, 39(1):

187-192, Feb. 1958. 2 figs. , table. DWB, DLC -Telemetering systems of the U. S. nonrecoverable satellites are designed

for direct observations in space, to record observations made

by the satellite's instruments, to encode such observations

for transmittal to ground stations and to accomplish the actual

transmission. In this U.S. -IGY program accuracy and reliability are the watch words and the embodiment of the transmission system is wrapped up in two packages, viz: the Lymanalpha and the cosmic ray packages, which are internationally

studied by a chain of stations in the U. S. , as well as at

strategic points over seas under a volunteer telemetering re- cording system. (Met. Abst. 12. 5-59. )--N. N.

D-510 Maxwell, Alan and Little, C.G. , A radio astronomical investi - gation of winds in the upper atmosphere. Nature, London,

169(4305) :746-747, May 3, 1952. 3 figs., 3 refs. DWBMeasurements of irregularities in radiation (80 Mc/s ) from

radio stars at 3 stations give winds in F layer at nighto

Histograms of direction and speed show, May-June, 60 N,

179
nearly all toward W-WNW, mean speed 250 km/hr; Sept. -Oct,

53°N, toward W-WSW, 430 km/hr. Rapid changes of speed

observed. (Met. Abst. 3. 10-200. )--C.E. P.B.

D-511 Maxwell, A. and Dagg, M. , A radio astronomical investigation of drift movements in the upper atmosphere. Philosophical Magazine, London, 45(365): 551 -569, June 1954. 7 figs.

,

6 tables, refs. DWB--Records of fading of 3. 7 m emissions

from Cygnus and Cassiopeia at night on three receivers near

Jodrell Bank showed irregularities in the diffracting screen at

about 400 km height indicating steady translation. Average

speed was 210 m/s, but ranged from - 1000. Direction was

nearly constant across magnetic lines of force, from W 19 h

to midnight, changing rapidly to E or ESE 1 - 4 h. Movements

are similar over a wide area, but in the F region in the auroral

zone the average drift is 360 m/s and the direction less constant, from W - SW 9 - 21 h, equally from SW or from E - SE

21 h - 6 h. A documented table of other evidence of F region

motion is given for comparison. (Met. Abst. 6D-250. )--

C E. P. B.

D-512 Maxwell, A. (Harvard Astronomy Sta. , Ft. Davis, Texas),

Radio emissions from the sun. National Electronics Conference, Chicago, Oct. 1957, Proceedings, Vol. 13:374-376,

pub. 1957 2 figs., 3 refs. DWB (621, 38 N277pr)--A brief

description of experiments at Ft. Davis, Texas (Harvard Radio

Astronomy Station) for recording radio frequency radiation from

sun at 100 - 580 Mc/s. Four distinct types of bursts are noted:

(1) long series of short bursts lasting hours or days (usually

below 250 Mc/s ), coming from solar corona or active sunspot

regions; (2) continuum radiation over a wide band, sometimes

after great bursts; (3) slow drift bursts, intense at first and

drifting toward lower frequencies, lasting 10 min and accompanied by visual flares; (4) fast drift bursts of a few seconds.

Over 9000 fast drift solar radio bursts were recorded in 14

months, associated with minor solar flares. (Met. Abst.

11.8-77.)-M.R.

D-513 Maxwell, A. ; Swarup, G. and Thompson, A. R. , The radio

spectrum of solar activity. Institute of Radio Engineers, N. Y.,

Proceedings, 46(1):142-149, Jan. 1958. 8 figs. , 2 tables, 9

refs., eqs. DLC- -Observations of the solar spectrum have

been made at the Harvard Radio Astronomy Station, Ft. Davis,

Texas, daily from sunrise to sunset since Sept. 1956. The

equipment comprises three separate receivers covering the

total range 100 - 580 Mc, and these are attached to a 28 ft diameter paraboloid antenna. The outputs of the receivers are displayed on intensity modulated, high resolution cathode ray

tubes, and these are photographed by a continuous motion

camera. Over all, the system is approximately ten times more

180
sensitive than any sweep frequency equipments used previously for solar observations. Examples of the records

showing the four main types of radiation from active areas

on the sun are given, and brief comments are made on the

existing theories to account for them. (Met. Abst. unpub. )--

Authors' abstract.

D-514 Maxwell, A ; Howard, W. E. , III and Garmire, G. (all,

Radio Astron. St. of Harvard Coll. Observ. , Ft. Davis, Texas),

Some statistics of solar radio bursts at sunspot maximum.

Journal of Geophysical Research, Wash., D. C. , 65(11):3581-

3588, Nov. 1960. fig., 7 tables, 8 refs. , eq. DWB, DLC--

This paper discusses the occurrence and intensity of solar

radio bursts at four frequencies in the band 100 to 600 Mc/s.

The observations cover 4010 hrs during a 12 month period at

sunspot maximum; the results refer essentially to bursts of

intensity greater than 10'21 mks unit and duration greater than

0. 3 sec. The statistical information is interpreted in terms of

the spectral characteristics of the bursts. The experimental

data were taken at Ft. Davis, Tex. , and the analysis shows

that at 125 Mc/s burst radiation was recorded for 560 hrs, of

which 380 hrs were of low intensity. At 200 Mc/s the burst

radiation covered 350 hrs, of which 240 hrs were of low intensity„ For these two frequencies the bursts occurred mainly in

the form of noise storms (spectral type I). At 425 and 550

Mc/s the total times of the solar bursts were much less, being

respectively 21 and 23 hrs; for the most part, however, this

radiation was of high intensity and appeared in the form of

continuum radiation (spectral type IV ) over a wide frequency

range. (Met. Abst. 11L-93. ) --Authors' abstract.

D-515 Mayer, C.H. ; McCullough, T. P. and Sloanaker, R.M. (all,

Radio Astronomy Branch, U. S. Naval Res. Lab. , Wash. , D. C. ), Measurements of planetary radiation at centimeter wavelengths . Institute of Radio Engineers, N. Y. , Proceedings, 46(1):260-

266, Jan. 1958. 5 figs. , table, 11 refs., 3 eqs. DLC--Radiation from the planets, Venus, Mars, and Jupiter, has been measured at wavelength of 3. 15 cm using the Naval Research Lab.

50 ft reflector and a narrow band radiometer. The apparent

blackbody temperatures for Mars and Jupiter derived from the

radio measurements agree reasonably well with the results of

infrared radiometric measurements. For the case of Venus,

the apparent blackbody temperature derived from the 3. 15 cm

measurements is about a factor or two higher than the value

derived from the infrared measurements. A measurement of

the radiation from Venus at 9. 4 cm wavelength was made using

the same antenna. The apparent blackbody temperature derived

from this measurement agreed well with the value derived from

the 3.. 15 cm measurement, but the accuracy of the 9. 4 cm re- sult was low because of the small flux density of radiation and

the small number of observations. (Met. Abst. 11. 6-143) —Author's

abstract,,

181
D-516 Mayer, H. F. (Cornell U. ,Sch. of Elec.Engr. ), Radio noise

considerations. Cornell Univ. School of Electrical Engineering

Contract W19-122 ac-41f Solar Noise Technical Report, No. 1,

Aug. 1949. 52 p. figs. , eqs. DWB—Three reports, based on

the author's lectures, are presented. The purpose is to lay the

groundwork for designing and building suitable radiometers for

solar noise observations. The first report is entitled Investigations of noise statistics ." in which is considered white noise

as a function of frequency and time. The second report, "Limitations by noise in solar noise measurements." treats six factors upon which the minimum detectable signal depends. The

third report: "Law of rectification, noise fluctuations and signal sensitivity" treats three factors with direct bearing upon

the subjects under discussion. (Met. Abst. 9A-9. )--W. N.

D-517 Mechtly, E. A. and Bowhill, S. A. (both, Ionos. Res. Lab.,

Penn. State Univ. ), Measured noise intensities on 512 Kc/s

frequency. Journal of Geophysical Research, Wash., D.C.,

65(10):3501, Oct. 1960. DLC--A rocket launched from the Air

Force Missile Center, Cape Canaveral, Florida, May 1959,

carried a pair of magnetic dipole antennas, turned to 512 kc/s,

each being connected to a receiver. The signal level at each

receiver was telemetered to ground level and recorded. The

range of height covered was from ground level to over 400 km,

following a somewhat oblique trajectory. The values of noise

intensities observed were found to depend critically on the

height region in the ionosphere. Below the ionosphere the measured intensities were 6. 8 x 10" l"? Watt m"2 (c/s)"l for antenna

A and 1. 2 x 10"!3 Watt m"2 (c/s)" 1

for antenna B. In the ionosphere, between 90 and 400 km height, the intensities for both

antennas remained essentially at the lower limit of measurability, about lO- 1^ Watt m"2 (c/s)" 1

. Above 400 km height, the

intensities on both antennas fluctuated widely, but in a similar manner, between the lower limit of measurability and an

upper limit corresponding to an equivalent free space intensity

of about 3 x 10-15 Watt m"2 (c/s)- 1 (Met. Abst. unpub. )--

E. Z. S.

D-518 Medd, W.J. and Covington, A.E. (both, Nat'l. Res. Council,

Ottawa, Canada), Discussion of 10. 7 cm solar radio flux measurements and an estimation of the accuracy of observations.

Institute of Radio Engineers, N. Y. , Proceedings, 46(1):112-

118, Jan. 1958. 5 figs., 2 tables, 12 refs. , 11 eqs. DLC--

The accuracy of the daily 10. 7 cm solar flux measurements

taken at the Nat'l. Research Council, Ottawa, has been investigated. The various system parameters are examined and

an auxiliary experiment, using a horn antenna, is described.

These studies lead to a revision of the early values of the

solar flux and require the use of conversion factors to some of

182
the published data. It has been estimated that the relative

error between observations separated by intervals of months

may be + 10% during 1947 through 1949, and + 3% during subsequent years. The systematic error in 1952-1953 was estimated at 7%. (Met. Abst. 11. 6-147. )--Authors' abstract,,

D-519 Medved, D.B. (Convair. Physics Section, San Diego, Calif. ),

Secondary electron emission and the satellite ionization phenomenon. Institute of Radio Engineers, N. Y. , Proceedings,

40(6): 1077-1078, June 1961. fig., 10 refs. , 4 eqs. DLC--

Outlines a model for ionization buildup based on secondary

electron emission from the surface of a satellite between 90

and 250 km and at > 1000 km. The plane parallel analysis

and the equations developed are shown to be valid for a cylindrical or spherical satellite. Variation of sheet thickness and

electron density as a function of altitude are plotted --W. N.

D-520 Meinel, A.B. (Kitt Peak Nat'l. Obs. , Tucson, Ariz.), Astronomical observations from space vehicles. Astronomical Society of the Pacific, San Francisco, Publications, 71(422):369-

380, Oct. 1959. DLC--An interesting discussion of the scope

and possibilities of astronomical observations from space vehicles. The requirements that a space telescope must meet and

the design problems are discussed. The discussion is divided

into two parts. The first part consists of astrophysical considerations. Eight general areas of fruitful research and discovery in space astronomy are enumerated. In the second section ten principal problem areas relative to engineering considerations for a space telescope are considered. (Met. Abst.

HL-29.)-I.S.

D-521 Menzel, Donald Howard, Our sun. Philadelphia, Blakiston,

1950. 326 p. 178 figs., 6 tables, refs. DWB--A beautifully

illustrated and handy textbook or reference work based on

years of research and survey literature in respect to the physical-chemical conditions of the sun and their effects on terrestrial atmospheric, magnetic and other geophysical phenomena. The results of basic research done during the war (1939-

1945) have, fortunately, been included. Discussions of interest to meteorologists include among others, those on auroras,

the production of ozone by UV radiation, long range forecasting based on solar influences, the sun's corona, cycles, climatic changes,, solar heating, effect of eclipses, magnetic

storms, sunspots, solar faculae, solar spectroscopy, radio

communication, ionospheric physics and last, and definitely

least, the poorly established relations between the sunspot

cycle and human behavior (economic and biological factors)

which the author maintains should be viewed with suspicion.

(Met. Abst. 3. 10-279. )-M.R.

183
D-522 Menzel, D. H. ; Warwick, James W. and Larence, Roberts.,

A dynamic spectrum analyzer for Sacramento Peak. Harvard

Univ. Harvard College Obs. Solar Dept. , Contract AF 19(604)-

146, Scientific Report, No. 20, Jan. 6, 1955. 12 p. 8 figs.

DWB--Analysis of optical observations of flares and associated

chromospheric activity emphasized the importance of building

at Sacramento Peak a dynamic radio spectrum analyzer similar

to that now in use at the Commonwealth Scientific and Industrial Research Organization near Sydney, Australia. Dynamic

spectra of the radio region, taken simultaneously with observations of associated optical activity, would provide a powerful

tool for study of many solar-terrestrial effects. In particular,

such an instrument promises to be of special value in studies

of magnetic and ionospheric storms, solar cosmic ray sources,

sudden ionospheric disturbances and the aurora borealis. Sec.

II of this report discusses the observations that support this

conclusion. Sec. Ill of the report analyzes the requirements

for a dynamic spectrum analyzer, with special reference to its

planned use in conjunction with optical observations, and es- tablishes general specifications for such equipment. The re- quirements imposed by the optical records have been coordinated with the limitations of electronics, so that the proposed

design is consistent with the present day techniques of radio

engineering. (Met. Abst. 7. 4-288. )- -Authors' abstract.

D-523 Menzel, D. H. and Krook, Max, On the origin of solar radio

noise. Harvard Univ. Obs. Solar Dept. , Contract AF 19(604)-

1394, Scientific Report No. 2, 1956. 4 p. DWB--This paper

discusses, in a general way, the problem of energy transport

when gas -kinetic processes dominate. Coupling exists between the material and radiation fields, with the result that

certain frequencies are amplified because the fundamental

equations are non-linear. The effects of density gradient, temperature gradient, etc. , are important because a disturbance

of small amplitude in a region of high density may grow to

large amplitude as it moves out through the solar atmosphere.

The presence of magnetic fields further complicates the situation, making possible the distinction between longitudinal and

transverse oscillations. The paper discusses the modes of

oscillation, the coupling of the different modes, the setting-up

of shock waves, and the possible conversion of mechanical

energy into the form of radio frequency emission. (Met. Abst.

9A-124.) -Authors' abstract.

D-524 Menzel, D. H. (ed. ), The radio noise spectrum. Cambridge,

Mass. , Harvard Univ. Press, 1960. Price: $7. 50. 183 p.

figs., tables, refs. , eqs. Contents (these articles abstracted

separately): Allen, E. W. , Man-made radio noise, p„ 1-6.

Peterson, Allen M. , The aurora and radio wave propagation,

p. 7-42. Lawrence, Robert S. , Ionospheric scintillation of

184
radio waves of extraterrestrial origin, p. 43-47. Eshleman,

Von R. , Meteor scatter, p. 49-78. Hawkins, Gerald S. # Electromagnetic emission from meteors, p. 79-92. Helliwell,

R.A„, Whistler-mode propagation, p. 93-100. Maxwell, A.;

Swarup, G. and Thompson, A. R. , Radio spectrum of solar

activity, p. 101-110. Aarons, Jules, Natural background

noise at very low frequencies, p. 111-122. Gold, Thomas and

Menzel, Donald H. , Solar whistlers, p. 123-128. Burke, B. F.,

Noise of planetary origin, p. 129-140. Bracewell, R.N. Correcting noise maps for beamwidth, p. 141-150. Menzel, Donald H. , Study on cosmic radio noise sources, p. 151-176.

Gold, Thomas, Interstellar hydrogen, p. 177-179. DWB (621.

38411 M55lra), DLC--The individual chapters of this book consist of papers presented by the respective authors at the Conference on Radio Noise held at Harvard College Observatory,

April 22, 1958. The studies deal with problems of radio noise,

its source, whether man made or natural, over the known range

of frequencies as well as the origins and significance of cer- tain characteristic noise radiations. Following the presentation of each paper discussions were held and pertinent parts of

the discussion are appended to the papers. (Met. Abst. 12„ 6-

l.)--E.Z.S.

D-525 Merrill, Harrison J. (Signal Corps Engr. Labs. , Ft. Monmouth,

N. J. ), Satellite tracking by electronic instrumentation. (In:

Van Allen, James A. (ed. ), Scientific uses of earth satellites.

Ann Arbor, Univ. of Michigan Press, 1956. p. 29-38. 2 figs.,

3 tables, 4 refs. ) DWB, DLC --Certain characteristics which

warrant consideration in the passive detection and tracking of

the satellite emphasize the usefulness of optical. techniques.

In planning for the use of existing equipment, it becomes apparent that there are essential differences between satellite

tracking and astronomical observations or missile tracking.

The problems associated with the satellite are due principally

to the diminished contrast against the sun illuminated sky and

to the tracking acceleration component and the concomitant

instrumentation jitter. Improvements in the optical compatibilities of the tracking and location instrumentation can be developed if combinations of electronic techniques are utilized

which have characteristics more suitable than photographic

film or the eye. These improvements are associated with su- perior time constants, background elimination, utilization of

the optimum spectral region, and the superior characteristics

of the electronics in the servo tracking loop. (Met. Abst.

9. 3-82. )--Author's abstract.

185
D-526 Merson, R.H. (Royal Aircraft Estab. , Farnborough, Hants,

Eng. ), Techniques of analyzing terrestrial radio and optical

observations of earth satellites. Astronautica Acta, Vienna,

5(l):26-39, 1959. 8 figs. , 2 tables, 5 refs. , eq. English,

German and French summaries p. 26. DWB. Also issued in

International Astronautical Congress, Amsterdam, Aug. 1958,

Proceedings of the 9th Congress, Vol. 2:828-841, issued

1959. 8 figs. , 2 tables, 5 refs. , eqs. English, German and

French summaries. DLC (TL787. 144) --After a brief description of the R. A. E. satellite prediction service and a short

section on Doppler measurements and their analysis, this

paper goes on to describe the main features of radio interferometer and kinetheodolite observations of satellite orbits made

by the staff of the Royal Aircraft Establishment. The development of a method of analyzing the observations on a digital

computer is given in broad outline, together with estimates of

the accuracy with which a satellite's position can be determined. A table of orbital elements of the second Russian satellite is included and a comparison is made between the theoretical and observed values of the rate of rotation of the or- bital plane. These differ by 0. 7% and indicate the possibility

of improving the accepted values for the coefficients in the

formula for the earth's gravitational potential field. (Met.

Abst. 11.9-148. ) -Author's abstract.

D-527 Metzger, P. G. and Strassl, H. (both, Bonn Univ. Obs.

,

Dept. of Radioastron. , Germany), The thermal radiation of

the moon at 1420 Mc/s . Planetary and Space Science, 1(3):

213-226, Aug. 1959. 4 figs. , 2 tables, 20 refs. , 17 eqs.

DLC --Measurements of the thermal radiation of the moon were

made with the continuum receiver of the 25 m radio telescope

at Bonn Univ. The observations and their reductions, covering three lunations (April 30 to July 22, 1958 ) are described

in detail. It was found that, within the working accuracy of

+ 2% relatively, the radiation temperature of the moon at 1420

Mc/s shows no variation with the phase of the moon. This

may be explained by the fact that the observed radiation has

its origin at some depth underneath the moon's surface where

the periodic variations of heating from the sun have become

insignificant. The mean value of the radiation temperature at

1420 Mc/s is found to be 250. 2 with an estimated absolute

uncertainty of about + 12%. --Authors' abstract.

D-528 Michigan. Univ. Engineering Research Institute, Atmospheric

phenomena at high altitudes. May 1 to July 31, 1957. Contract DA-26 -039 SC -64659, Quarterly Report, Oct. 1957. 38 p.

10 figs. (incl. photos), 9 tables, forms, 4 refs. DWB (M10. 5

M624ad)--Two grenade Aerobee rockets were flown successfully at Ft. Churchill in July. Data reduction and analysis of

reccvds on SMI: 01 has continued. Theoretical studies have

186
continued on the subjects of the explosion produced modulation of DOVAP records, finite amplitude of propagation effects,

the effect of variation in velocity of propagation of electromagnetic radiation on the DOVAP system, the possibility of measuring ambient pressure at very high altitudes, and the dynamics of rarefied gases. (Met. Abst. 9. 7-151. )--Authors' abstract.

D-529 Mickelwait, Aubrey B. ; Tompkins, Edwin H. , Jr. and Park,

Robert A. , Interplanetary navigation. Scientific American,

N.Y., 202(3):64-73, March 1960. 16 figs. DWB, DLC--

A discussion of the practical prospect of interplanetary flight

in the light of recent satellite launchings. The next step in

space flight will be for the rockets to bring the payload close

to — or even land them upon — another planet. This requires

difficult compromises among the conflicting demands of payload, radio communication, guidance and available power.

This paper presents a systematic and extensively illustrated

discussion of these problems of interplanetary navigation.

(Met, Abst. 11. 12-479. )--I.S.

D-530 Millman, George H. (General Elec. Co. , Syracuse, N. Y. ),

Analysis of tropospheric. ionospheric and extraterrestrial effects on VHF and UHF propagation. General Electric Co.

Electronics Div. , Technical Information Series, R56EMH31,

Oct. 6, 1956. 138 p. 68 figs. , tables, 50 refs. , numerous

eqs. Photostat copy. DWB (M94. 7 M655an) -Effects of the

atmosphere and extraterrestrial noise sources on the propagation of VHF and UHF radio waves are discussed. Relationships are derived for calculating refraction effects, time delays, Doppler errors, polarization changes and attenuation of

radio waves traversing the atmosphere. These conclusions

were reached. Refraction and time delay effects in the troposphere are independent of frequency and are a direct function of

relative humidity in the air. In the ionosphere refraction and

time delay errors, polarization shift and attenuation are inversely proportional to the square of frequency. The Doppler

frequency error in the troposphere is directly proportional to

frequency while in the ionosphere is inversely proportional to

frequency. The theoretical total radiation from the quiet sun,

in the radio frequency spectrum, is directly proportional to

frequency raised to about the 0. 755 power. The total flux

density emanating from radio stars, Cassiopea and Cyguus,

is inversely proportional to the frequency raised to the 0.81

power. (Met. Abst. 11E-99. )—Author's abstract.

187
D-531 Millman, G. H. , Atmospheric effects on VHF and UHF pro- pagation. Institute of Radio Engineers, Proceedings, 46(8):

1492-1501, Aug. 1958. 16 figs. , 4 refs. , 53 eqs. DLC, DWB

—This report discusses the effects of the troposphere and ionosphere on the propagation of VHF and UHF radio waves. In

order to accurately calculate the refraction effects, time delays, Doppler errors, polarization changes and the attenuation experienced by radio waves traversing the entire atmosphere, the author has derived some mathematical relationships.

Tropospheric refractive index profiles and ionospheric electron

density models representative of average atmospheric conditions are also presented in this paper. (Met. Abst. 11E-100.

)

--N. N.

D-532 Mimno, Harry Rowe, The physics of the ionosphere. Reviews

of Modern Physics, 9(l):l-43, Jan. 1937. 16 figs., 309 refs.,

24 eqs. DLC --This important paper opens with a brief historical survey followed by a simple analysis of the more prominent features that distinguish the components of the radio spectrum. A more detailed discussion includes following topics,

among others: thunderstorms and barometric effects, local

ionospheric clouds, scattering and interaction of radio waves,

etc. It is concluded that the complex physical system re- quires study by statistical methods. The classical magnetoionic theory* or rather the anomalies, is considered. The

molecular atomic ionization and recombination processes

await a generally accepted theory explaining the stratification of the ionosphere. (Met. Abst. 6D-12. )--W. N.

D-533 Miner, Richard Y. (Arma Div. , Amc. Bosch Arma Corp.

,

Garden City, N. Y. ), Experimental observation of space

vehicles. Navigation, Los Angeles, 6(4): 252-263, 1959.

9 figs. , 7 refs. DWB, DLC -The purpose of this article is to

stimulate the interest in visual and radio observations of rockets and satellites. The observational requirements of both

methods are itemized and the application of instruments and

other devices are described. Procedures of forecasting and

subsequent conversion to apparent position and time are ex- plained including the use of and the plotting on charts and

coordinate system grids, etc. (Met. Abst. 11. 9-147. )--W. N.

D-534 Minnis, CM. (Radio Research Station, Slough), The F2

layer during eclipses of 1952. 1954. and 1955. (In: Solar

eclipses and the ionosphere: a symposium. . . ed. by W. J. G.

Beynon and G. M.Brown. London, Pergamon, 1956. p. 81-84.

2 figs. , table, 8 refs. ) DWB--It is desirable that the electron

density as a function of height in the F2 layer should, where

possible, be computed, because the changes in foF2 alone

during an eclipse can give a misleading impression of the

response of the layer to the drop in incident radiation intensity,

188
At Khartoum in 1952, foF2 remained almost constant for two

hours during the eclipse, although there were marked changes

in electron density at constant height at all levels. Assuming

that these changes can be accounted for by an attachment process, values of the attachment coefficient have been derived

which are similar to those obtained by SAVTTT at Bocayuvo.

The great height of the layer at Khartoum has allowed values

to be computed for heights up to 400 km. The small difference

between foFl and foF2 at Inverness and Slough in 1954 has

made it difficult to deduce the shape and true height of the F2

layer. After allowing for the retardation due to the Fl layer,

it is concluded that the observed fall in foF2 was not accompanied by any appreciable change in the height or thickness

of the F2 layer. The attachment coefficient determined for the

peak of the F2 layer was considerably smaller than the values

obtained at Bocayuvo and Khartoum for the same height. (Met.

Abst. 9. 3-278. )--Author's abstract.

D-535 Minnis, CM. (D.S.I. R. Radio Research Station, Slough),

The interpretation of changes in the E and Fl layers during

solar eclipses. Journal of Atmospheric and Terrestrial Physics,

N.Y., 12(4):272-^o2, 1958. 5 figs., 2 tables, 22 refs. , 4

eqs. DLC --Recent eclipse measurements have been explained

in terms of the response of a Chapman layer to the obscuration

of a solar disk on which localized sources of ionizing radiation are superposed on a uniformly bright background. This

interpretation is supported by several features of the results

obtained during a series of eclipses, An alternative interpretation postulates a complex layer containing two different

species of ion but assumes only a uniformly bright solar disk.

This hypothesis has been examined but calculations based on

it result in expected changes in the layer, during an eclipse,

which are not in accord with certain characteristics of the ex- perimental data. A suggestion has been made that the layer

tilts which occur during an eclipse may give rise to errors in

the interpretation of the data. Experimental results are quoted

which suggest that such errors probably are not important.

(Met. Abst. 10.4-300. ) -Author's abstract.

D-536 Minnis, C. M. (Dept. of Sci. and Indus. Res. , Radio Res.

Station, Slough), Solar activity and the ionosphere. Nature,

London, 181(4608):543-544, Feb. 22, 1958. ref. DWB, DLC--

Sunspot cycles are not associated with any appreciable change

in the amount of visible light and heat radiation emitted by the

sun; but they increase the intensity of the ultraviolet and Xradiation which is responsible for the existence of the E layer

of the ionosphere. As compared with 1954, the intensity of

ultraviolet and X-radiation had increased threefold in 1957.

Similar estimates of the intensity of the F2 layer confirm the

conclusions reached using the E layer results. The large

189
changes in the intensity of the ionizing radiation associated

with the sunspot cycle produce corresponding variations in the

structure and electron density of the layers of the atmosphere

and influence the propagation of radio waves. During Oct.

1957f radio stations in the U. S. could be received in England

on frequencies of 37. 5 Mc/sec in the early afternoon. Even

near sunspot in 1954, instances were not uncommon in which

European radio stations, operating in the very high frequency

band, interferred with television and other radio signals in

southern England. An examination of the twenty sunspot cycles which have occurred since 1749, shows that the present

one and its predecessor must be regarded as having maxima

which are well above the average. (Met. Abst. 10.1-337.)--

LL.D.

D-537 Minnis, CM. and Bazzard, G.H. (both, D. S. I. R. Radio

Res. Station, Slough), Some indices of solar activity based

on ionospheric and radio noise measurements. Journal of

Atmospheric and Terrestrial Physics, N. Y. , 14(3/4): 213-228,

June 1959. 5 figs. , 4 tables (in appendix), 10 refs. ,17+4

eqs. DWB, DLC--The critical frequencies of the E and F2 lay- ers of the ionosphere are closely controlled by the level of

solar activity but, at any fixed point on the earth's surface,

they also vary with season owing to the annual change in the

solar zenith angle. A .critical frequency can only be used to

provide an index of solar activity if such seasonal variations

can be eliminated or reduced to very small proportions. Methods of achieving this are described and monthly mean values

of an E and an F2 layer index are tabulated for the period 1938-

1957. The correlation of these indices with each other and

with the solar noise flux at .A 10. 7 cm is high. Some possible practical applications of such indices are discussed

briefly. (Met. Abst. 11F-88. )--Authors' abstract.

D-538 Minnis, CM. and Bazzard, G.H. (both, DSIR Radio Res.

Station, Slough), A monthly ionospheric index of solar activity based on F2 layer ionization at eleven stations. Journal

of Atmospheric and Terrestrial Physics, London, 18(4):297-

305, Aug. 1960. fig.. Stables, 6 refs. , 3 eqs. DLC--

A monthly index has been constructed for the period 1938 to

date, using monthly mean or median noon values of foF2 at

eleven widely distributed stations. The correlation between

foF2 at noon and this index is significantly greater than that

between foF2 and either the 3 month weighted mean sunspot

number or the monthly mean solar radio noise flux at 2800

Mc/s. Numerical estimates have been made of the errors incurred in forecasting noon and midnight foF2 several months

ahead using these three indices as guides to the trend of solar

activity. (Met. Abst. 11. 12-403. ) -Authors' abstract.

190
D-539 Minnis, C. M. (Radio Res. Station, Slough, Bucks), An

estimate of the peak sunspot number in 1968. Nature, London,

186(4723) :462, May 7, 1960. 4 refs. DWB-The operating conditions of high frequency radio communication links are profoundly modified by changes in solar activity. It is of importance, therefore, to estimate the probable limits within which

the forthcoming peaki sunspot number will lie. From the study

of the length of sequences of uninterrupted increases and decreases it is possible to estimate the probability of occurrences.

The probability of a fourth increase higher in 1968 than in 1958

is approximately 0. 3. The range of values can be estimated

from the frequency distribution of the observed peaks as from

the differences between successive peaks. It was found that

the 1968 peak will be in the range 110-160. (Met. Abst. 11L253J--E.K.

D-540 Minnis, CM. and Bazzard, G.H. (both, DSIR Radio Res.

Station, Slough), A world-wide semi-annual cycle in the E

layer of the ionosphere. Journal of Atmospheric and Terrestrial

Physics, London, 18(4):306-308, Aug. 1960. fig., 4 refs.

DLC--A study of the E layer character figure for eight stations

in the north and south hemispheres has disclosed an unexpected semi-annual cycle, the variations in which have the same

sign in both hemispheres. The amplitude of the cycle is about

+ 15% near the maximum of the solar cycle but vanishes at the

minimum. Its origin has not yet been discovered but several

possibilities are discussed, (Met. Abst. 11.12-382.)--

Authors' abstract.

D-541 Mitra, A. P. and Jones, R.E. (both, Penna. State College,

Ionosphere Research Lab. ), Determination of the location of

the ionospheric current system responsible for geomagnetic ef- fects of solar flares. Journal of Atmospheric and Terrestrial

Physics, London, 4(4/5): 141-147, 1953. 2 figs. , 2 tables,

23 refs. , 2 eqs. DWB--A new method for locating the ionospheric current system associated with solar flares is presented.

The method depends on the time of maximum intensity of a geomagnetic flare effect and the enhancement of electron density

at the relevant level. It is found that the flare current system

is located either at 100-130 km (if one assumes that the flare

effect is essentially one of enhancement of the Sq current) or

at 60 km (if it is an independent system). (Met. Abst. 11D100. )- -Authors' abstract.

D-542 Mitra, A. P. , Ionospheric effects of solar flares, Pt. 1, Evalua - tion of experimental data. Penn. State Univ. Ionosphere Res.

Lab., Contract AF 19(604) -3875, Scientific Report No. 112,

Oct. 15, 1958. 57 p. 23 figs. , 7 tables, 26 refs. , 42 eqs.

(Pt. 2, in Sci. Report, No. 113) DWB--

191
This is the first of a series of reports dealing with the ionospheric effects of solar flares. The present work describes the

various radio and magnetic data and deals with initial methods

of analysis. These include long and short radio wave absorption, change in phase height and, to a lesser extent, group

height measurements. Magnetic crochets are also treated

from the viewpoint of the current systems by which they are produced. (Met. Abst. 11D-101. ) —Author's abstract.

D-543 Mitra, A. P. (Div. of Radiophysics, C. S.I. R.O. , Australia),

Study of the ionosphere by extraterrestrial radio waves. Indian

Journal of Physics, Calcutta, 26(10):495-511, Oct. 1952. 3

tables, 7 figs. , refs. p. 510-511. DLC--The paper presents

a comprehensive review of a novel method of studying the ionosphere in which the radio frequency radiations from extraterrestrial sources may be utilized. Four different types of measurements of such waves are discussed for this purpose, namely: 1) ionospheric refraction, 2) ionospheric attenuation,

3) twinkling of "radio stars" and 4) effects of sudden ionospheric disturbances (SID's). The available experimental re- sults are compared with ionospheric theory and further lines

of investigation which might profitably be followed are indicated. (Met. Abst. 5.5-90.) -Author's abstract.

D-544 Mitra, A. P. , The lunar semi-diurnal oscillation in the ionospheric absorption of 150 kc/s radio waves. Journal of Atmospheric and Terrestrial Physics, 7(1/2): 99-100, Aug. 1955.

2 figs. , 3 refs. DWB--Harmonic dials are presented for lunar

semidiurnal oscillations in Pennsylvania for day (D region)

and night (E region). Day oscillation is only about 0. 1 km,

maximum 4 hrs after lunar transit. Night oscillation is 0. 20

(2f+80°) km. (Met. Abst. 7. 1-186. )-C. E. P.B.

D-545 Mitra, A. P. (Commonwealth Sci. and Industr. Res. Org.

,

Div. of Radiophysics, Australia) and Shain, C.A. (Univ. of

Calcutta, Inst, of Radiophys. and Electronics, India), The

measurement of ionospheric absorption using observations of

18. 3 Mc/s cosmic radio noise. Journal of Atmospheric and

Terrestrial Physics, London, 4(4/5): 204-218, 1953. 12 figs.,

3 tables, 18 refs. DW6--A new technique permits measurement of the total attenuation suffered by 18. 3 Mc/s cosmic

radio noise passing completely through the ionosphere. It is

shown that the total absorption may be divided into two components, one due to absorption mainly in the D region and the

other in the F2 region. The observations of D region absorption confirm the diurnal and seasonal variations observed by

other workers. F2 absorption depends on the critical frequency but not on the height of the region and there is evidence

of increased absorption at night which may be caused by irregularities in the upper F region. The observational results are

192
compared with those obtained by other workers and suggestions are made for the use of the method, particularly in the

exploration of the upper F2 region. (Met. Abst. HE-101.)--

Authors* abstract.

D-546 Mitra, S. K. , The story of radio electronics. Journal of Scientific and Industrial Research, Sec. A, New Delhi, 14(1):3-13,

Jan. 1955. 6 footnotes (incl. 3 foot-refs. ). DWB-This presidential address to the 42nd Session of the Indian Science

Congress, Baroda, Jan. 4, 1955, opens with a brief summary

of radio electronics from fundamental research to practical

applications in radio climatology, radio astronomy and defense.

Next part takes up India's position in radio research, facilities

and future. It ends with an appeal to the younger generation to

take advantage of study facilities in the nationally important

field of radio electronics. (Met. Abst. 7. 7-67. )—W. N.

D-547 Mitra, S. K. (Prof, of Physics, Calcutta Univ. ), The upper

atmosphere. 2nd ed. Calcutta, The Asiatic Society, (preface

1952. ) 713 p. figs. , tables, bibliog. p. 644-668, eqs. DLC,

MH-BH--The first edition of this valuable work, published in

1947, contained 616 pages. About 100 pages of new material

have been added, including the results of the latest research

in almost every field covered by the 13 chapters. These additions include work on escape of atmospheric gases (Chap. I),

atmospheric tides (Chap. II), radar studies of meteors (Chap.

Ill), variations in ozone content with latitude and air masses

(Chap. IV), dissociation of Np (Chap. V), ionospheric sounding by radio waves, estimation of recombination coefficients,

tides and traveling disturbances in the ionosphere (Chap. VI),

Sq and L = variations near the geomagnetic equator (Chap. VII),

up-to-date bands and lines in auroral spectrum (Chap. VIII),

new theories of magnetic storms and aurora by ALFVEN and

MARTYN (extension of Chapman-Ferraro theory) (Chap. IX),

Russian work on zodiacal light and afterglow or airglow, height

measurements of luminescent layers, hydrogen and sodium in

the upper atmosphere, etc. (Chap. X), revised model of temperature distribution in upper atmosphere (GERSON) (Chap. XI),

a new chapter on rocket exploration of upper atmosphere (V-2

and aerobee flights) (Chap. XII), and new unsolved problems

of the upper atmosphere (Chap. XIII). Brief discussion of

winds at high levels from indirect methods (Chap. XIII). No

attempt at listing all of the important subjects covered in this

work would do justice to its comprehensiveness. The amount

of carefully prepared illustrative material (charts, graphs,

tables, schematic diagrams, etc. ) both borrowed and original,

is amazing. In most cases the sources are carefully cited and

a class bibliography of nearly 1000 references is a further aid

in locating source material on all fields of upper air research

by physical methods. (Met. Abst. 4. 8-15. )--M. R.

193
D-548 Mitra, S. N. (All-India Radio, New Delhi), Partial solar

eclipse of Feb. 25. 1952. and its effect on the ionosphere. Journal of Scientific and Industrial Research, Sec. A, 12(7):

319-328, July 1953. 6 figs. , table, 7 refs. DWB--Ionospheric observations taken by the All-India Radio from Feb. 20

to March 1, 1952, at Delhi, Bombay, Madras, Tiruchirapalli

and Nagpur, India, are reported. The observations comprised

(1) vertical incidence ionospheric measurements; (2) relative

field intensity observations; (3) observations of fading and

back scatter on pulsed transmissions at Delhi; (4) observations on pulsed transmissions emitted from England; and (5)

photographing the sun's disk at regular intervals. Graphs

giving the measured values are presented and discussed.

(Met. Abst. 6. 1-52. )--G.T.

D-549 Miyazaki, Yukio and Takeuchi, Hajime (Inst, of Physical

and Chemical Research, Tokyo), Altitude dependence and

time variation of the radiation intensity observed by U. S.

Satellite 1958 CO. Japan. Science Council. Ionosphere Research Committee, Report of Ionosphere Research in Japan,

12(4):448-458, 1958. 6 figs. , table, 6 refs. DWB, DLC--

Telemetering signals from the U. S. Satellite 1958 ttpassing

near Japan were analyzed (cosmic rays). The results are as

follows: 1) As the altitude increased from 340 km to 1200 km,

the counting rate of a single G-M counter mounted in the satellite showed a gradual rise and above 1200 km a steep rise.

The altitude curve also showed appreciable day-to-day variation which masked the latitude dependence of the intensity

between 12 to 24 geomagnetic latitude. 2) The altitude

curve seemed to show a comparatively wide hump at about

350 to 800 km. 3) Dividing the data into a certain narrow

range of latitude and altitude, the counting rate increased

gradually day by day from Feb. 1 to Feb. 10, 1958. Finally,

it reached a value factor 2 greater than the earlier one. While

in this period, the planetary magnetic index K

p was also increasing but its fine variation did not always correspond to

that of the counting rate. The variation of the radiation intensity at higher altitude seemed to have an appreciably longer

time constant than that of the geomagnetic fluctuation. 4) On

Feb. 11, the enhancement of the radiation intensity was observed at an altitude of about 1000 km. The time of onset

was inferred to be between 0640 and 0842 UT. The neutron

intensity of cosmic rays observed at sea level or at mountain

altitude showed an increase in the neighborhood of 0700 UT.

(Met. Abst. 12. 5-119.) -Authors' abstract.

194
D-550 Miller, F. , Atmospheric water vapor measurements at 6-7

microns from a satellite. Planetary and Space Science, 5(3):

202-206, July 1961. fig. , 5 tables, 4 refs. , 3 eqs. DLC--

A theoretical estimate of the changes of radiation expected

under a variety of atmospheric structures is presented and discussed. Temperature measurements, by means of satellites, are non-conclusive since water vapor changes with temperature,

but are valid for the non-temperature radiation of carbon dioxide. -W. N.

D-551 Moody, Alton B. , Navigation using signals from high altitude

satellites. Institute of Radio Engineers, N. Y. , Proceedings,

48(4): 500-506, April 1960. 3 figs. (incl. photo). DLC-If

electronics can be satisfactorily applied to celestial navigation, a system having universal coverage without weather limitations might be produced. Radio stars are not a promising

possibility, but the sun and moon are being tracked by the U.S.

Navy Radio Sextant, AN/SRN-4, to provide limited coverage.

Universal coverage might be achieved by the addition of artificial earth satellites. Satellites in orbits a few hundred miles

from the earth might be used in some form of piloting system,

but orbit prediction problems, limited coverage by individual

satellites, and computer complexities are serious obstacles to

be overcome by such a system. A different approach would be

to place three or four satellites in orbits at an optimum distance somewhere between 1000 and 12, 000 miles from earth to

serve as artificial celestial bodies in a system that would be

natural evolution from traditional celestial navigation methods.

A stabilized directional antenna, operating with a receiver

capable of accepting signals from both the satellites and the

sun, would provide angle measurement data both for fixing the

position of the craft and also for establishing a north reference.

The degree of sophistication of the user equipment would differ

with requirements. (Met. Abst. 11. 12-590. ) --Author's abstract.

D-552 Mook, Conrad P. (Diamond Ordnance Fuze Labs. , Wash. , D. C. ) and Johnson, David S. (U. S. W. B. ), Proposed weather radar

and beacon system for use with meteorological earth satellites.

Reprint from 1959 Conference Proceedings, 3rd National Convention on Military Electronics, Institute of Radio Engineers,

Professional Group on Military Electronics. (1959). p. 206-

209. 2 figs. , 4 refs. , 2 eqs. DWB (M08. 77 M817pro) -Resolution, wave length selection, receiver sensitivity, power and

antenna requirements are some of the factors that must be taken

into consideration in designing a meteorological satellite radar

system. These five factors are discussed in terms of application to rainfall return. It is concluded that a satellite mounted

radar is much preferred to other satellite weather surveillance

systems. It provides three dimensional synoptic coverage of

195
world wide rainfall patterns on a round-the-clock basis. Other

surface weather elements such as pressure and wind can also

be read from remote automatic beacon type weather stations.

(Met. Abst. 11M10.)--N. N.

D-553 Moorcroft, D. R. (Radio Physics Lab. , Defence Res. Board,

Ottawa), Radio tracking; of earth satellites . American Journal

of Physics, N. Y. , 27(2):73-86, Feb. 1959. 17 figs. , 24 refs.,

71 eqs. DWB--The characteristics of artificial earth satellite

orbits are summarized and related to an observer on the sur- face of the earth. Equations and analytical approaches are developed for determining the orbit of a transmitting satellite

using information from equipment for measuring the Doppler

shift of the transmitted signal. These are extended to include

observations with an array of interferometers (several different

arrangements are considered). (Met. Abst. 11.9-149.)--

Author's abstract.

D-554 Morgan, M. G. and Johnson, W. C. (both, Hanover, N. H. ),

Preliminary results from the U. S. I. G. Y. "Whistlers-East"

program. (In: International Scientific Radio Union. IGY Committee, Some Ionospheric results obtained during the IGY.

Amsterdam, Elevier, 1961. p. 386-387). DWB, DLC--Preliminary experimental data received from 13 stations situated in a meridional chain along 70 W and stretching from the Arctic

to the Antarctic, showed that the whistlers echo back and

forth between the hemispheres. Properties of the whistlers

were described. The associated ionospherics showed a 13-

day period of activity and exhibited different characteristics

with latitude, as well as a preference to certain hours of the

day. (Met. Abst. unpub. )--S. N.

D-555 Mullard Radio Astronomy Obs. , Cambridge, England, Radio

observations of the Russian earth satellite. Nature, London,

180(4592) :879-883, Nov. 2, 1957. 9 figs. , 2 refs. DWBInterferometer observations of track on 20, 40 and 80 Mc/s

are described and an approximate orbit derived. Variations

in intensity of received signal were due to various causes.

Presence of a transmitter at varying zenith angles and various

heights offers new methods of ionosphere investigation and

preliminary results have been obtained. Estimates of density

of atmosphere, etc., were also made. (Met. Abst. 9.2-99.)

--C. E. P. B.

D-556 Muller, C. A. (Radio Obs. , Dwingeloo, Netherlands), 21 cm

hydrogen line absorption in the spectra of discrete sources.

(In: Paris Symposium on Radio Astronomy, July-Aug. 1958,

(Proceedings), pub. Stanford Univ. Press, 1959. p. 360-365.

5 figs. , table, 6 refs. ) DLC--

196
A short survey of the results obtained with the Dwingeloo

25 meter radio telescope (beamwidth 56) and the 21 cm

receiver on hydrogen line absorption effects in the spectra

for a number of strong point sources. The emission profile

and absorption profile are discussed. The individual sources

considered are: Cassibpeia A, Taurus A, Cygnus A, Orion

A, Virgo A, and also Sagittarius A. A table lists the absorption components in four bright sources. (Met. Abst.

unpub. )--£. Z. S.

D-557 Muller, Hans-Gerhard, Messmethoden in der Radioastronomie. (Measurement methods in radio astronomy. ) Zeitschrift

fur Instrumentenkunde, Brunswick, 68(6): 117-124, June 1960.

16 figs. , 6 refs. DWB--Today radio astronomy is an independent branch of science. Although the aims are essentially

similar to those in optical astronomy, different techniques

are required in the radio range. The fundamental problems

and measuring procedures are dealt with in this review.

(Met. Abst. 11. 12-40. )--Author's abstract.

D-558 Muller, Rolf; Augustin, Otto; Menzel, Willi and others,

Solare und terrestrische Beobachtunqen wihrend des MdgelDellinqer-Effektes (SID) am 19. November 1949. (Solar and

terrestrial observations during the Mogel-Dellinger effect

(SID) on Nov. 19, 1949. ) Journal of Atmospheric and Terrestrial Physics, l(l):37-48, 1950. 9 figs. , table, 18 refs.

MH-BH--A bright chromosphere eruption began Nov. 19, 1949

at 10 h 34 min. Cosmic radiation shown by ionizing effect

or counter coincidences at several stations increased by 10-

20% in 10-20 min, confirming earlier observations. Echo

soundings on 1-16 MHz gave no reflection from E layer and

none from F at lower frequencies. Echoes on 1800 KHz

failed at 10:30 and field strength of transmission on 6078. 9

KHz from 400 km fell nearly to zero at 10. 50. Geomagnetism

showed no special disturbance so that slow corpuscles from

the eruption failed to reach the earth. (Met. Abst. 2. 9-66. ) --C. E. P. B.

D-559 Munro, G. H. (Radio Res. Board Lab. , Univ. of Sydney),

Diurnal lapse of signals from Sputnik III . Nature, 183(4674):

1549, May 30, 1959. ref. DLC. (Comment by) B. G. Pressey.

Ibid, 184(4682), Suppl. No. 5:261, July 25, 1959. DLC--

Munro reports observations made at Blaxland, near Sydney,

Australia of radio signals from Satellite 1958 5 2. These

were started shortly after the satellite started orbiting in May

1958. No definite failure of signal was observed until early

March 1959; since that time, however, there have been definite lapses of modulation. These lapses occur when the

satellite is not illuminated by the sun. Even in the absence

of pulse modulation, a weak background signal can be

197
detected on close transits. PRESSEY reports observations

made at Slough, England, and at Singapore, which confirm

the absence of pulse signals during darkness, but show no

evidence of the background signal observed in Australia.

(Met. Abst. 11. 12-566. )--G.T.

D-560 Munro, G. H. (Radio Res. Lab. , Electrical Eng. Dept. , Univ.

of Sydney), Ionospheric information from satellite signals.

Nature, London, 187(4742): 1017 -1018, Sept. 17, 1960. 2 figs.,

3 refs. DLC --Observations of fading rates of signals from satellites have been analyzed for various observing sites and fading rate profiles have been built up. These are converted to

ionization profiles by comparison with corresponding ionosonde

recordings. Results derived from various satellites for a two

year period are illustrated diagrammatically. The difference

between the summer and winter distributions is marked. The

main purpose of this paper is to report the remarkable result

in Sept. 1958 when the rate increased practically from summer

to winter values within two days when the satellite was at a height of 400 km. These results are also illustrated diagrammatically. (Met. Abst. 11. 12-374. )--R.B.

D-561 Munro, G. H. and White, R.B. (both. Radio Res. Lab., c/o

Elec. Eng. Dept. , Univ. of Sydney), Observations in Australia of radio transmission from the first artificial earth satellite . Nature, London, 181(4602): 104, Jan. 11, 1958. 2 figs.

DWB--The Radio Research Board in Australia has had a choice

of 20 and 40 Mc/s for radio transmissions from the first Soviet

satellite which has provided a new approach to the study of the

ionosphere. In order to record the intensity variations of the

signals from these satellites the Overseas Telecommunication

Commission provided a low noise site and good receiving facilities at Bringelly, near Sydney. This material tells how the

observational procedures were carried out. (Met. Abst. 10. 9-

104.)-N.N.

D-562 Munro, G. H. and Heisler, L. H. (both. Radio Res. Bd.

,

Sydney Univ. ), Recording radio signals from earth satellites . Nature, London, 183(4664) :809-810, March 21, 1959. fig.

,

ref. DWB--A simple and very satisfactory Doppler frequency

shift system developed at the radio laboratory at the Univ. of

Sydney is described and discussed. The total Doppler shift of

20, 005 Mc/s is 1000 cycles. One of the many good features

of the recording system is the accuracy by which the slope of

the Doppler shift curve 3F/ 2t is derived at the point of

closest approach. Dependency of rate of change of ^F/ ?t

on h (height) and V (velocity) of the satellite enables V/h

curves to be derived (by a Siliac computer) for the overhead

case and one other transit, intersection of which establishes

198
the satellite's velocity and height. Facsimile record of signals from Sputnik III is given and the analysis of recordings

since the end of August is now in process. (Met. Abst.

11. 12-565. )--W. N.

D-563 Murcray, W. B. and Pope, J. H. (both, Geophysical Inst.

Univ. of Alaska, College, Alaska), Doppler shifted cyclotron frequency radiation from protons in the exosphere. Physical Review Letters, N.Y., 4(l):5-6, Jan. 1960. 2 figs. , 2

refs. DLC--This paper investigates in detail a suggestion by

T. W. MacARTHUR, in a recent publication, (see ref. D-4833

that the phenomenon known as "Dawn chorus" may be due to

Doppler shifted radiation from protons which are rotating about

the lines of force of the earth's magnetic field with the cyclotron frequency: Vc

= 1. 54 x 1()3 3 , where 3 is the field

strength in gauss. Theoretical chorus dispersion curve and

audio spectrogram of chorus illustrate the discussion. (Met.

Abst. 11. 12-319. )-I.S.

D-564 Murcray, W. B. and Pope, J. H. (both. Geophysical Inst.

Univ. of Alaska), Energy fluxes from the cyclotron radiation

model of VLF radio emission. Institute of Radio Engineers,

N.Y., Proceedings, 49(4):811-812, April 1961. 5 foot -refs. -- This brief discussion on the mechanism of "Dawn chorus" involves the works by Santirocco and other workers. Santirocco's

recent calculations of the energy radiated by gyrating protons

in the earth's magnetic field are interesting but not convincing;

neither is the travelling wave amplification hypothesis. (Met.

Abst. unpub. )--W. N.

D-565 Murray, W. A. S. and Hargreaves, J. K. , Lunar radio echoes

and the Faraday effect in the ionosphere . Nature, London,

173(4411) :944-945, May 15, 1954. 2 figs. , 2 refs. , eq.

DLC--Observations on 120 Mc/s at Jodrell Bank show that

long period (about 60 min) fading of echoes from the moon is

due to rotation of polarization. This is attributed to change

of mean electron density in the ionosphere. (Met. Abst. 8. 8-

172.)--C.E,P.B.

D-566 Nagoya, (Japan} Univ. Research Institute of Atmospherics,

Data on solar radio emission with some notes. Nagoya. Univ.

Research Institute of Atmospherics, Proceedings, 4:90-129,

Dec. 1956. 3 figs. , mostly tables. DWB--Observations made

at 3750 Mc/s and 9400 Mc/s with radiometers first put into

operation in Nov. 1955 and used since May 1956 for routine

observations 6 hrs a day. Attenuation due to thin clouds

proved negligible, but that due to nimbus was as much as 40%.

Results are given in extensive tables, curves, and scatter diagrams. Bursts prominent at 9400Mc/s were seen on Dec. 20,

1956. The daily flux density at the 2 frequencies has a

199
correlation coefficient of + 0. 95 and the 5 component at 9044

Mc is 0. 8 of that at 3750 Mc/s. Observations with an 8 element interferometer have been made 5 hrs a day since Nov.

1956. A burst sometimes occurs in a region where no intense

radiation is usually observed. (Met. Abst. 9A-125. )--M. R.

D-567 Nagoya, Japan. Univ. Research Institute of Atmospherics,

IGY data on atmospherics, whistlers and solar radio emissions.

Vol. 2-3. Jan. 1 -June 30 and July 1 -Dec. 31. 1958. Issued

Feb. and June 1959. About 250 p. each. Entirely tables.

"Compiled by the Research Institute of Atmospherics, Nagoya

Univ. " --The contents are as follows: 1. reports of atmospherics and whistlers, sferics network during IGY and operating schedule; 2. atmospheric average intensity, integrated

intensity of atmospheric radio noise, monthly average and

sudden enhancement of atmospherics; 3. intensity of

atmospheric radio noise, hourly value: db( luv/m^Odb), (median intensity during 10 min from 50 min to 00 min in each

hour); 4. atmospheric noise recording ( WMO, Recommendation 40, 1957-CAe), whole year of 1958 between lat 34°50'N

and long. 137 22'E; 5. monthly return for narrow sector bearing (the same as above); 6. atmospheric radio noise data by

statistical method, noise field intensity and cumulative amplitude probability distribution in percent and diurnal variation

of noise intensity; 7. sferics fixes and wave forms of atmospherics (only in December for three different stations); 8.

whistler data, 8 classified designators by whistler, magnitude of the dispersions (185 p. ) and 9 solar radio emissions,

intensity and polarization at frequencies of 9400, 3750, 2000

and 1000 Mc/s, flux density. (Met. Abst. 12. 7-28. )--K. C.

D-568 Naismith, R. (Dept. of Scientific and Industrial Research,

Slough), Solar activity and radio communication. Nature,

London, 181(4614) :954-956, April 5, 1958. 3 figs. DWB--

The period 1957-1958, one of highest solar activity within the

past 200 yrs was chosen for the International Geophysical

Year as most appropriate for observations of radio communication. The major events of the program of the Radio Research

Board are reported here. Sunspot number for Dec. 1957 was

244. The monthly median value of foF2 at noon at Slough during December was 15. 2 Mc/s the longest in 26 yrs. The maximum frequency available for the longest distance radio communication at the latitude of Slough is close to 50 Mc/s at

noon for half the days in the month. This can be applied in

the planning of radio communication in the temperate regions.

(Met. Abst. 11E-106.)--N.N.

200
Narasinga Rao, K.V. ; Verdeyen, J. T. and Goldstein, L.

(all, Dept. of Elec. Eng. , Univ. Illinois), Interaction" of

microwaves in gaseous plasmas immersed in magnetic fields . Institute of Radio Engineers, N. Y. , Proceedings, 49(12):

1877-1889, Dec. 1961. 18 figs. , 20 refs. , 29 eqs. DLC--

The phenomenon of radio frequency electromagnetic wave

interaction in gaseous plasmas is reviewed. The application of microwave interaction to the study of plasmas immersed in magnetic fields is discussed. Attention is

focused on the effects produced in such plasmas when one

of the simultaneously propagating microwaves is in electron cyclotron resonance. It is demonstrated that for relatively modest amplitudes of the resonating wave, the kinetic energy of the electrons increases considerably, which

in turn, affects (1) the electron collision frequency, and

(2) the magnetic field control of the plasma confinement.

(Met. Abst. unpub. )- -Authors' abstract.

National Research Council. United States National Committee on International Scientific Radio Union (ISRU),

Report on the 12th General Assembly, Aug. 22-Sept. 5,

1957, Boulder, Colo. National Research Council, Publication, No. 581, 1958. 195 p. figs. , Mimeo. DWB

(621.384 N277 re), DLC (TK5700. 1834). This report

on General Assembly also issued in Institute of Radio

Engineers, Proceedings, 46(7): 1350-1383, July 1958. -- The 7 reports cover: 1) Radio measurements and standards by Ernst Weber; 2) Tropospheric propagation by

John B. Smyth; 3) Ionospheric propagation by L. S. Manning; 4) Radio noise of terrestrial origin (sferics and

whistlers) by Harold E. Dinger; 5) Radio astronomy by

F. T. Haddock; 6) Radio waves and circuits by E. C.

Jordan; 7) Radio electronics by W. G. Shepherd. The

12th General Assembly of I. R. S. I. at Boulder was attended by over 500 radio scientists from 26 countries. The re- ports provide an excellent summary of work going on all

over the world in each field. The agenda for the 7 ses- sions is given on p. 1350-51 by FREDERIC H. DICKSON,

and U. R.S.I, and its officers and chairman are discussed

on p. 1351-2 by H. W. WELLS. The address of welcome

by DETLEV W. BRONK, President of the National Academy

of Sciences, appears on p. 1352-4. The extensive report

on the Academy of Science contains notes on attendance,

program, detailed transactions of the assembly, symposia

and business sessions, documents, discussions, resolutions, etc. (Met. Abst. 11. 1-22. )--M. R.

201
D-571 National Research Council, Wash. , D. C. U. S. National

Committee on the International Scientific Radio Union

(URSI), Symposium of the Exosphere and Upper F Region,

May 4. 1960. National Bureau of Standards, Wash. . D. C.

Journal of Geophysical Research, Wash., D. C. , 65(9):2563-

2636, Sept. 1960. (Summaries of papers, or full manuscript

in case of papers to be published in near future. ) DWB--A

report of the proceedings of the Symposium is presented. The

contributions fall into the following four categories: general

feature of the exosphere and upper F region; electron densities in and above the F region as revealed by magnetoionic

refractive effects imposed on radio emissions from rockets

and artificial satellites; integrated electron content derived

from refractive effects; electron-ion densities and temperatures derived from incoherent backscatter. Papers from these

four groups with the corresponding discussions are summarized in a fifth section. (Met. Abst. 12. 6-3. )--0. T.

D-572 National Research Council, Wash. , D. C. U. S. National

Committee on the International Scientific Radio Union,

Report of U. S. Commission 3 on Ionospheric Radio Propagation, to the 13th General Assembly of the' ISRU, London,

Sept. 5-15, 1960. U. S. National Bureau of Standards, Journal of Research, Sec. D, 64(6):629-636, Nov. /Dec. 1960.

Bibliog. p. 634-636. DWB, DLC-This review of U. S. activities and progress in the field of ionospheric radio propagation between Jan. 1957 and Dec. 1959, is arranged as follows:

Structure of the upper atmosphere; ionizing radiations; electron densities; satellite beacon studies; ionospheric processes; ionospheric disturbances; sporadic E and spread F;

studies of the lower ionosphere; radar studies of auroral ionization; refraction in the ionosphere; ionospheric propagation studies; ionospheric scatter transmissions and radio

reflection from meteor ionization; ionospheric propagation

research with communication systems applications. An ex- cellent bibliography of current material, arranged alphabetically by authors, is included. (Met. Abst. 12. 8-112. )«W. N.

D-573 National Research Council, Wash. , D. C. U. S. National

Committee on the International Scientific Radio Union, Report

of U. S. Commission 4 on Radio Noise of Terrestrial Origin, to

the 13th General Assembly of the ISRU. London. Sept. 5-15.

1960. U. S. National Bureau of Standards, Journal of Research,

Sec. D, 64(6): 637-654, Nov. /Dec. 1960. Bibliog; p. 652-

654. DWB, DLC-This critical review of U. S. research activities 1957-1960 includes a bibliography of current material and

the following papers: Radio frequency radiation from lightning

discharges; properties of atmospheric noise at various receiving locations; summary of research on whistlers and related

202
phenomena; a summary of VLF and ELF propagation research;

hydromagnetic waves and ELF oscillation in the ionosphere

and the exosphere. (Met. Abst. 12. 8-114. )--W. N.

D-574 National Research Council. U. S. National Committee on the

International Scientific Radio Union, Report of U. S. Commission 5 on Radio Astronomy, to the 13th General Assembly of

the ISRU. London, Sept. 5-15. 1960. U. S. National Bureau of

Standards, Journal of Research, Sec. D, 64(6):655-669, Nov./

Dec. 1960. Bibliog. p. 667-669. "Review of developments

occurring within the U.S. in the field of radio astronomy."

DWB, DLC--Highlights of developments and activities (1957-

1960) in radio astronomy in the U. S. are evaluated separately

for each of the following research centers: Univ. of Alabama;

Sagamore Hill Radio Astronomy Observatory; U. S. Army Signal Research and Development Lab. ; California Inst, of Tech.,

Owens Valley Radio Obs. ; Carnegie Inst, of Washington,

Dept. of Terr. Magnetism; Cornell Univ. ; Collins Radio Co.;

Univ. of Colorado High Altitude Obs. ; Harvard Univ. Radio

Astronomy Station; Hayden Planetarium; Univ. of Illinois;

U. S. Naval Res. Lab. , Radio Astronomy Branch; National

Aeronautics and Space Admin. ; NBS Boulder Lab. ; Nat'l.

Radio Astronomy Obs. ; Ohio State Univ. ; Rensselaer Polytech. Inst. ; Stanford Univ. ; Yale Univ. and Univ. of Michigan. The report is complemented by the current references to

each of the several topics considered. (Met. Abst. 11L-75. ) -W. N.

D-575 National Research Council, Wash. , D. C. U. S. National

Committee of the International Scientific Radio Union, Report

on the 13th General Assembly, Sept. 5-15, 1960, London,

England. National Research Council, Wash., D. C. , Publication 880, 1961. 5S5 p. figs. , tables, refs. , eqs. Price:

$5. 00 from National Research Council, Wash. , D. C. Contents:

Presidential Address. Address of President-elect, Smith-Rose;

Program of general Assembly. Actions of General Assembly.

List of delegates. Reports of the seven Commissions, Radio

Standards and methods of measurements. II. Tropospheric

radio propagation. III. Ionospheric radio propagation. IV.

Radio noise of terrestrial origin. V. Radio Astronomy. VI.

Radio waves and circuits. VII. Radio electronics. The following articles arranged here alphabetically by authors, were

classified respectively in the report under the above subject

headings: Bailey, Dana K. , Ionospheric "forward" scattering,

p. 281-286. Berkner, Lloyd V. , Science in space, p. 27-37.

Bolton, J. G. , The discrete sources of cosmic radio emission,

p. 407-436. Briggs, B.H. , Ionospheric drifts, p. 298-317.

Crawford, Arthur B. , Experimental results from investigations

on wave propagation through the troposphere, p. 95-107.

203
Haddock, Fred T. , Radio sources at 3 and 1. 8 cm wavelengths,

p. 462-472. Hey, J. S. , Radio astronomical observations of

planets, comets and meteors, p. 510-519. Hines, C. O. , Theoretical survey of motions in the ionosphere, p. 320-328. Little,

C. Gordon, Radio properties of aurorae, p. 261-270. Mayer,

Cornell H. ; McCullough, T. P. and Sloanaker, R. M. , Radio

Source polarization measurements at 11 cm, p. 457-462.

Owren, Leif, High latitude radio aurora observed at College,

Alaska, p. 272-275. Palmer, H. P. , The angular diameters

of radio sources, p. 437-440. Ryle, M. , Studies of galactic

sources at 178 Mc, p. 441. Schmerling, Erwein R. , Some

results of an I. G. Y. true height survey, p. 193-194. Seddon,

J. Carl, Summary of rocket and satellite observations related

to the ionosphere, p. 233-249. Sloanaker, R. M. and Nichols,

J. H. , Measurements of bright celestial sources at a wavelength of 10. 2 cm, p. 453-457. Smith, Ernest K. , Jr. , Morphology of sporadic E, p. 218-228. Smith, F. G. , Application of low noise receivers to radio, p. 486-496. Storey,

L. R.O. , "Whistler theory" -- Survey paper, p. 351-373. Thomas/

J. O. , Electron density distribution in the ionosphere, p. 188-

192. Watkins, C. D. , Auroral radio-echo observations at

Jodrell Bank, p. 270-272. Westerhout, G. , Galactic radiation and its physical interpretation, p. 473-483. Wrigley, F.

Craig, K. J. and Yaple, B. S. , Parametric amplifiers in radar

astronomy, p. 496-502. (Met. Abst. unpub. )--W. N.

D-576 Nelson, J. H. , Planetary position effect on short wave signal

quality. Electrical Engineering, 71(5) :421 -424, May 1952.

figs. , table, 4 refs. DLC--Correlation over seven years established author's hypothesis that certain planetary positions affect short wave signals. Possibly (particularly in the case of

multicycles) the influence of solar planets on the sun will

cause temporary changes in the sun's characteristic radiation

which is registered by the ionosphere, apparently sensitive

to these changes. Based on solar observation, planetary indications and a day-to-day signal analysis, the 24 hr forecasting system developed by the RCA Communication Inc. , aver- aged close to 85% throughout 1950 and 1951. (Met. Abst.

6. 3-344.) -W.N.

D-577 Nesmeianov, A. N. , Vselennaia raskryvaet svoi tainy: issledovanie kosmicheskoqo prostranstva s pomoshch'iu raket i sputnikov. (The universe reveals its secrets: investigations

of cosmic space by means of rockets and satellites. ) Pravda,

Moscow, 48(196, i. e. 14, 955):3-4, July 15, 1959. photo,

8 figs. "Report issued by A. N. Nesmeianov, pres. of the

Akad. Nauk. March 1959". DLC (Slavic R. R. )--A substantial and official report of the "informative" type giving details

of progress in cosmic ray, radio propagation, ionosphere,

micrometeorite, magnetic, interplanetary gases, belt of high

204
D-578

radiation, upper atmosphere, composition, density, ionization (electron and positive ion concentration), and biological

research in space and, finally, basic concepts for cosmic

flights, as gained from the 3 Soviet "Sputniks" and later space

probe flights. A number of graphs showing quantitative re- sults in the above fields are included. (Met. Abst. 10. 10-90. ) -M.R.

Netherlands. Meteorologisch Instituut, Het Internationaal

Geophysisch Jaar. 1957-1958. (International Geophysical

Year, 1957/1958. ) Its Verspreide Opstellen, No. 4, 1957.

79 p. figs., photos. Contents: Vening Meinesz, F. A. : Algemene inleiding (Introduction), p. 7-16; Bleeker, W. : Het budget van de dampkring, (Atmospheric budget), p. 17-

23; Groen, P. : Het onderzoek van de wereldzee, (Oceanographic research), p. 25-31; Veldkamp, J. : De hoogste

luchtlagen, (The upper layers of the atmosphere), p. 33-41;

Minnaert, M. G. J. : De waarneming van de zon, (Solar observations), p. 43-48; Jongen, H. F. : De kosmische straling,

(Cosmic rays), p. 49-55; DeVoogt, A. H. : Het radioverkeer

in het International Geophysisch Jaar, (Radio propagation),

p. 57-63; Roelofs, R. : Aarde, maan en sterren, (The earth,

moon and stars), p. 65-70; Oort, J. H. : Kunstmatige satellieten, (Artificial satellites), p. 71-79. DWB--This attractive

brochure consists of 9 articles on different phases of the IGY,

with frequent reference to participation by the Netherlands.

The preface is by C. J. WARNERS, director of the KNMI (Netherlands Meteorological Service). The illustrations vividly depict

vp-rious IGY activities. (Met. Abst. 9. 9-44. )--M. R.

D-579 Netherlands. Telecommunications Services, The Hague.

Ionosphere and Radio Astronomy Section, A remarkable solar

radio event. Nature, London, 181(4608):542-543, Feb. 22,

1958. fig. , ref. DWB, DLC--A discussion of a large increase

in solar radio noises observed on Nov. 4, 1957, on a frequency

of 200 Mc/sec at the receiving station "Nera" of the Netherlands Telecommunications Services. The increase started suddenly at 0848 U. T. and lasted for more than 5 hrs; at its greatest intensity it amounted to some 900 times the noise level of

the quiet sun. The smoothed intensity level showed considerable fluctuations with periods of the order of a few minutes.

There was no report of the occurrence of a solar flare near the

onset of the radio event; nor was a sudden ionospheric disturbance observed. It was also observed at 169 Mc/sec at Humain

(Belgium) and Nancy (France) but was entirely absent on the

decimeter-centimeter wavelength range and on a wavelength

near 6 meters. "The radiation was 100% left-handed circularly

polarized. The position of its source, as determined at 1125

U. T. with a two-element interferometer, was about 0. 1 solar

radius east of the center of the solar disk 1 The unusual

205
character of this great radio phenomenon was particularly

evident from records obtained with a negligible time constant.

Such records are reproduced. Their analysis reveals short

period fluctuations of intensity, with a period of 0. 2-0. 3 sec

of a type hitherto unobserved. Part of this variability showed

an oscillatory type of intensity fluctuation; in other parts decreases in intensity and short dips of a fading character predominated. During the later stages of the radio event dips

and oscillations of the order of 0. 1 mm occurred. No ionospheric oscillations of radio sources of any importance were

observed at Jodrell Bank on Nov. 4. Hence, the very short

period of intensity fluctuations must also be attributed to

solar conditions. This peculiar type of variability is revealed

only by a recording instrument with a time constant no greater

than a very small fraction of a second. The occurrence of

fluctuations in intensity characterizing this solar radio event

suggests that in special circumstances, solar coronal gas may

produce scintillation effects possibly analogous to ionospheric

scintillations but more analogous in character. (Met. Abst.

unpub. )--I. L. D.

D-580 Newell, Homer E. , Jr. (Naval Res. Lab. , Wash. , D. C. ),

international Geophysical Year earth satellite program. Franklin Institute, Phila. , Journal of the Franklin Institute Monographs, No. 2:2-13, June 1956. DWB--Details of Project Vanguard, including instrumentation of vehicle by Navy Research

Lab. , and the 11 ton launching vehicle being constructed by

Glenn L. Martin Co. ; orbit, 3 stage performance, optical and

radio observing program, computational centers and geophysical or astrophysical problems which may be solved by the

earth satellite program are discussed in this article. (Met.

Abst. 9.4-45.)--M.R.

D-581 Newell, H. E. , Jr. (National Aeronautics and Space Admin. ),

The United States programme in space research. Royal Society

of London, Proceedings, Ser. A, 253(1275):538-541, Dec. 29,

1959. DWB--The National Aeronautics and Space Administration (NASA), created by the National Aeronautics and Space

Act in 1958, plans to continue the use of sounding rockets

and satellites in exploring the earth's atmosphere and the

space beyond. Some of the areas of major scientific interest

include: atmosphere, ionosphere, high energy particles, fields

(gravitational, magnetic, electric), photons, astronomy and

controlled experiments. (Met. Abst. 11. 12-457. )--E. K.

206
D-582 Newton, H. W. and Piggott, W. R. , Observational aspects

of solar corpuscular radiation. International Council of Scientific Unions, Brussels, Eighth Report of the Commission

for the Study of Solar and Terrestrial Relationships. Paris,

1954. p. 101-111. fig. , tables, 86 refs. DWB--Observations of flares and magnetic storms during the declining phase

of the last sunspot cycle are listed. The solar phenomena, es- pecially radio noise, accompanying the emission of corpuscular streams, the direct detection of such streams and their effects on the ionosphere, aurora, geomagnetism, etc. , are discussed. (Met. Abst. 91-45. )--C. E. P. B.

D-583 Newton, H. W. , Face of the sun. London, Harmondsworth:

Penguin Books, 1958. 208 p. 37 figs. , 15 refs. Price:

2 sh 6 d. DLC (QB521. N4). Review by C. W. Allen in Science Progress, London, 47(186):344-345, April 1959. Review

by H. C. Shellard in Weather, London, 14(7):238, July 1959. -- A thorough, popular science monograph on all aspects of solar

surface phenomena and their important effects on the terrestrial

atmosphere: magnetic storms,the aurora, radio propagation

(ionosphere) and weather, rainfall and tree rings, from an historical, as' well as a modern (e. g. , IGY program) viewpoint.

The photosphere, chromosphere, corona, sunspots, solar rotation, spectroscopy, cycles of 11 yrs, Zurich numbers and

Greenwich areas, characteristics of sunspots, magnetic field

theories, giant sunspots (1859, 1892, 1921, 1926, 1946, 1947),

the 25 biggest sunspots, flares and prominences, geomagnetic

records and disturbances, radio waves and cosmic rays from

the sun, aurora, weather "cycles, " solar constant, cosmology,

and stars outside our system are considered. Numerous plates

and drawings and a good subject index are included. It is odd

that the 5 greatest (of 25) sunspots in 70 years (1874-1954) oc- curred in 6 years (1946-1951). (Met. Abst. 10. 11-30. )--M.R.

D-584 Nicolet, Marcel, Les observations scientifiques a l'aide des

satellites artificiels. (Scientific observations by means of

artificial satellites. ) Belgium. Institut Royal Meteorologique,

Contributions, No. 46, 1959. 7 p. DLC. Reprinted from

Societe Royale Beige des Ingenieurs et des Industrials, (Publication?), No. 12:527-533, 1958. --The author describes ac- curately the data gathered at the present time by observation

of the three artificial satellites launched, and indicates what

results may be expected. The assumptions advanced regarding composition of the atmosphere seem to be confirmed through

the observations of satellites. These are the only conclusions

that can be drawn up to now. The other data which may be ex- pected to be obtained are indicated as well as the methods used

for this purpose. There are two problems for which the use of

satellites is very useful: 1) the analysis of the energy spectrum

, of cosmic radiation with regard to latitude in the course of one

207
cycle of solar activity through an orbit crossing the poles;

2) the distribution of the lines of force of the earth's magnetic field, at great distance, could be investigated through

examining the change in intensity. Advantage of artificial

satellites over rockets is enormous. In spite of the large

number of rockets fired, these could only supply observations

for a total of 24 hrs, and in this total there are only 10 min of

observation at an altitude higher than 200 km. The great difficulty with satellites is their return to earth. (Met. Abst.

10. 10-93.) -A. V.

D-585 Nicolet, M. , Nouvelles de l'espace. (Space news. ) Ciel

et Terre, Brussels, 75(3/4):91-107, March/April 1959. 4

figs. DLC--Account of the results obtained by means of artificial satellites during the International Geophysical Year as

concerns high atmosphere. First of all, author discusses dissociation and recombination of oxygen and nitrogen molecules

in upper atmosphere, where motions of charged particles are bound to the earth's magnetic field. A table shows the main

peculiarities of the satellites launched up to March 1959.

Diminution of satellite's orbit, owing to decrease of speed

caused by atmospheric density, is discussed. The proportion

of change in satellite's orbit shows that the irregularities in

density of air result principally from fluctuations in solar ra- diation. Data relating to the changes in density within thermosphere and influence of the rise of temperature upon the increase in density are given. Densities observed and their

fluctuations show that the thermal gradient at 150 km is > 10

per km and may reach values such as 30 and 40 per km. Results obtained by means of satellites and whistlers show that

ionization decreases very slowly with altitude beyond the

maximum, in the range of 10^ electrons per cm^ , of the F2

region. They show that there is no propagation about the

equator and that the phenomenon follows the lines of force

going from one hemisphere to the other. Comments on the

artificial geomagnetic and radio electric effects caused

through thermonuclear explosions, and more particularly on

the artificial creation of temporary radiation zones at altitudes of 10, 000 km or so are included. (Met. Abst. 11. 4-

150. )--A. V.

D-586 Nicolet, M. (Royal Met. Inst. , Brussels) and Aikin, A. C.

(Penn. State Univ. ), The formation of the D region of the

ionosphere. Journal of Geophysical Research, Wash. , D. C.

,

65(5): 1469-1483, May 1960. 4 figs. , 6 tables, 52 refs. , 36

eqs. DLC. Also issued as Pennsylvania. State Univ. Ionosphere Research Lab. , Contract AF 19(604) -4563, Scientific

Report No. 125, Nov. 1, 1959. 40 p. 4 figs. , 47 refs. , 30

eqs. DWB (M10. 535.P415i)--

208
Radiations of solar origin penetrating below 85 km in the terrestrial atmosphere are: (1) X-rays of r < 10 A; (2) Lyman- alpha and (3) Wavelengths greater than 1800 A. These radiations can ionize: (1) molecular nitrogen and oxygen; (2) nitric

oxide and (3) metallic ions such as sodium and calcium. Molecular oxygen and nitrogen are also ionized by cosmic rays.

The negative ion to electron ratio is important below 70 km

and affects the electron distribution below that altitude.

Normal ionization conditions are explained by cosmic rays

and Lyman-alpha. Solar flare conditions are explained by x- rays. Above 85 km, the behavior of the ionization is related

to the E layer. (Met. Abst. 11F-97. )-Author's abstract.

D-587 Nisbet, John S. , Electron densities in the upper ionosphere

from rocket measurements. Pennsylvania. State Univ. Ionosphere Research Lab. , Contract AF 19(604) -4563, Scientific

Report No. 126, Dec. 10, 1959. 163 p. 51 figs. , 10 tables,

77 refs. numerous eqs. DWB (M 10. 535. P415i) -An investigation of electron densities in the upper F region of the ionosphere by new techniques employing long range rockets is described. Investigations were confined to propagation measurements between the missiles and ground stations, and to methods not requiring radio links with the missile in addition to

those already incorporated for telemetry and tracking purposes.

The types of rockets used for the tests were determined by the

requirement that suitable transmitters were carried, and that

the maximum rocket altitude allowed sufficient penetration of

the F region. In practice, this limited the vehicles to those

with satellite launch missions, and to intermediate range ballistic missiles. Since such vehicles have considerable horizontal velocity components, it was necessary to develop suitable methods of analysis. A matrix method is described for

analyzing oblique dispersion measurements to provide vertical

electron density height profiles. In this method, account is

taken of horizontal gradients, refraction, and the varying ray

path zenith angles in the ionosphere. Two methods of measuring ionospheric dispersion were employed and compared: Faraday rotation, and a method using the difference between the

apparent positions of the missile obtained by two tracking systems operating on different frequencies. Faraday rotation measurements at two receiving stations and on two frequencies

were compared, to check the horizontal gradient program and

the polarization of the rocket antenna. Results are given for

seven experiments of electron densities and electron contents

above the maximum ionization level of the F region. These

are compared with results of other investigations and some con- clusions are drawn about the structure of the layer and its diurnal variation. (Met. Abst. 1 IF-98. )- -Author's abstract.

209
D-588 Nordo, Jack, Solaktiviteten og dens innflytelse pa atmosfaeren. (Solar activity and its influence upon the atmosphere.)

Naturen, Bergen, 78(6): 175- 192, 1954. 10 figs. DWB--Various theories on the formation and activities of sunspots, particularly in relation to radio communication and weather, are reviewed. Solar flares are explained as hydrogen explosions

giving rise to considerable ultraviolet radiation. No significant influence of flares on air pressure was found (during the

17 yr period) in Norway, but a weak increase in summer and

decrease in winter was noticed in Oslo during the eruptions.

(Met. Abst. 6. 2-323. )-W. N.

D-589 Obayashi, Tatsuzo (Radio Res. Lab.), A possibility of the

long distance HF propagation along the exospheric field aligned

ionizations. Japan. Science Council. Ionosphere Research

Committee, Report of Ionosphere and Space Research in Japan,

13(3): 177- 186, 1959. 9 figs. , 7 refs. , 10 eqs. DWB, DLC--

Transequatorial very long range echoes of the order of 7000 km

detected by the HF backscatter sounder at Hiraiso are interpreted as the ground backscatter propagation launched on the

path along the exospheric field aligned ionizations. Ray path

calculation on this longitudinal mode of propagation between

the geomagnetically conjugate points along its field line is

made for various geomagnetic latitudes. The expected echo

distance agrees well with that obtained by the experiments.

It is also found that the average exospheric electron density

deduced from the observed echo spreads is about 10^ -^ 10^

electrons per cm^. A possible use of this propagation mode

of backscatter as a tool of exospheric sounding is suggested.

(Met. Abst. 11. 12-435. ) -Author's abstract.

D-590 Obayashi, T. (Radio Res. Lab. ), Entry of high energy particles into the polar ionosphere. Japan. Science Council.

Ionosphere Research Committee, Report of Ionosphere and

Space Research in Japan, 13(3):201-219, 1959. 14 figs. , 23

refs. , 37 eqs. DWB, DLC--An explanation is given for two

types of enhanced ionizations in the polar ionosphere associated with geomagnetic storms, viz. , the polar cap blackouts

and the auroral zone blackouts. The former appears several

hours after major type IV radio outbursts, yet, well before the

onset of geomagnetic storms, while the latter is closely re- lated to geomagnetic disturbances and auroral displays. It is

shoxvn that the polar cap blackouts are caused by the invasion

of energetic protons of 10 *~ 100 MeV produced in the solar

corona by an agitated plasma bearing magnetic fields, and that

these particles precipitate into polar ionosphere following

nearly the Stormer orbits. For the auroral zone blackouts, an

improved version of Stormer' s theory is applied, in which interesting behavior of a charged particle in the distorted geomagnetic field is revealed. The remarkable equatorward shifting

210
of the auroral zone and world wide increases of cosmic ray

intensity during the main phase of geomagnetic storms are explained consistently by the decrease of geomagnetic cutoff for incoming particles owing to the contraction of the geomagnetic cavity. (Met. Abst. 11. 12-428. ) --Author's abstract.

D-591 Obayashi, T. , Very low frequency spectra of atmospherics

propagated through the ionosphere. Nature, London, 184

(4679):34-36, July 4, 1959. 3 figs. , 7 refs. DWB--A more

complete experimental proof of the mode theory in very low

frequency ionospheric propagation and on the characteristics

of the atmospherics is given. Descriptive and experimental

facts are presented from the observations of atmospherics at

Ibaragiken, Japan. Typical records are examined. Among the

facts that lend support to the mode theory is the relation between the sudden enhancement of atmospherics and the sudden

ionospheric disturbances. (Met. Abst. 11E-109. )--W. N.

D-592 Obayashi, T. and Hakura, Yukio (both, Radio Res. Labs.

,

Kokubunji, Tokyo), Enhanced ionization in the polar ionosphere associated with geomagnetic storms. Journal of Atmospheric and Terrestrial Physics, London, 18(2/3): 101-122, June

1960. 11 figs. , 21 refs. , 15 eqs. DLC--New evidence indicating the existence of energetic solar particles associated

with solar flares has been found from the analysis of worldwide data of fmin *n the ionograms. An outstanding enhancement of ionization in the lower ionosphere occurs in the polar

region with a delay of several hours after a large solar flare

accompanied with major radio bursts of type IV. Radio blackouts due to enhanced ionizations develop, spreading inside

the whole polar cap without inducing any marked geomagnetic

activity. With the onset of a geomagnetic storm, however,

the blackout region spreads from the polar cap up to the so- called auroral zone. As the Dst field of geomagnetic storm

develops, it comes down to considerably low latitudes forming a spiral shaped ionization pattern. The radio blackouts,

which precede the onset of geomagnetic storms, may be termed

the polar cap blackouts because they are confined within the

geomagnetic latitude of about 60-65 , while those related to

geomagnetic storms and auroral displays are the auroral zone

blackouts. It is shown that the polar cap blackouts are caused by the invasion of energetic particles of the order of 10-

100 MeV, generated in an agitated solar coronal plasma bearing magnetic fields, and that those particles precipitate in the

polar ionosphere following nearly the Stormer orbits. For the

auroral zone blackouts, an improved version of the Stolrmer

theory is applied, in which an interesting behavior of a charged particle in the distorted geomagnetic field is revealed.

The remarkable equatorward shifting of the auroral zone and

some peculiar increases of cosmic ray intensity during the

211
main phase of magnetic storms are explained consistently by

the decrease of geomagnetic cut-off for incoming particles

owing to the contraction of the geomagnetic cavity. (Met.

Abst. 11. 12-425.)--Authors' abstract.

D-593 Obayashi, T. and Hakura, Y. (both. Radio Res. Lab.

,

Kokubunji, Tokyo), Polar ionospheric disturbances and solar

corpuscular emissions. Planetary and Space Science, N. Y.

,

5(l):59-69, Jan. 1961. 4 figs. , 3 tables, 24 refs. , 10 eqs.

DWB--It has been found that the study of polar radio blackouts

due to abnormal ionization in the lower ionosphere yields considerable evidence indicating the existence of energetic solar

particle associated with solar flares. Polar radio blackouts

are classified into two characteristic types, one is the polar

cap blackout and the other is the auroral zone blackout. It is

shown that the polar cap blackout appears with some hours delay after a major solar radio outburst of type IV, and the blackout is confined within the geomagnetic latitude of 60-65 . The

estimated energies of particles causing this are about 10-100

MeV. The auroral zone blackout then follows, being accompanied with geomagnetic storms and aurorae, and it may be

caused by the so-called auroral particles of 1 MeV or less.

The energy spectrum of solar particles associated with solar

flares is revealed from the present result together with all information from various -observations related to solar and terrestrial disturbances. It is concluded that solar particles have a conspicuous superthermal non -Maxwell ian tail extending from

a few keV up to relativistic energy range, through the bulk of

corpuscular clouds consists of rather low energy particles and

hence, likely to be in the Maxwellian distribution. Some discussions on the nature of solar corpuscular clouds and their

effect upon the terrestrial ionosphere are also given. --Authors

abstract.

D-594 Ordway, F.I. ,111 (General Astronautics Corp. , 11 W. 42nd St.,

N. Y. 36), Instrumentation of artificial satellites . Astronautica Acta, Vienna, 4(1):90-110, 1958. 21 figs. , 53 refs.

DWB--This investigation is mainly on the different instruments

installed in rockets and in earth satellites. Some four new instrument packages have been developed, laboratory tested and

approved. A description of each of these is included, plus

some descriptive work on meteoric erosion experiments, cosmic

ray observations, the investigation of the radiation balance of

the earth, the measurement of interplanetary matter and the satellite environmental measurements of pressure, temperature,

meteoric incidence and skin erosion. (Met. Abst. 10. 6-92.

)

--N. N.

212
D-595 Osborne, C.B. , Magnetic and radio disturbance. North Atlantic Ocean. Marine Observer, 22(156): 66-68, 1952. DWB--

June 17, 1951, magnetic compass varied several degrees from

gyro compass, during passage of a large sunspot. No radio

signals could be received. Reports on disturbances from Admiralty Compass Obs. , Overseas Telecommunications Dept.

of G. P. O. and Central Forecasting Office, Dunstable, are included. (Met. Abst. 6D-130.)-C.E.P.B.

D-596 Ovenden, Michael W. , The astronomical uses of small artificial satellites. Science Progress, London, 44(175):472-479,

July 1956. refs. DWB--The artificial satellite project is discussed. Satellites could give data of density of atmosphere

at heights of 100-300 mi, improve geodetic and gravity data,

measure electric current -density in the ionosphere especially

during solar flares, and give data of primary cosmic radiation

and the solar spectrum. The power problem may be solved by

solar batteries; other technical problems are discussed. (Met.

Abst. 7. 10-46.)-C.E.P.B.

D-597 Owren, Leif (Carnegie Inst. , Wash., D. C), Observations of

radio emission from the sun at 200 Mc/sec and their relation to

solar disk features. Cornell Univ. School of Electrical Engineering, Contract N6onr-264(06), Radio Astronomy Report, No.

15, May 1, 1954. 219 p. 32 figs. (incl. photos). 5 p. refs.

appended. DWB--A voluminous report giving results of solar

radio frequency radiation observations at 200 Mc/sec, from

April 1950-Dec. 1952, with a radiometer and radio interferometer at McMath-Hulburt and at Cornell Univ. Observatories.

Measurement of random noise, actual radiometer observations,

and radio interferometer observations in relation to solar features comprise the first 3 chapters (Pt. I). Pt. II consists of

two chapters covering radio emissions associated with solar

flares, and enhanced emission associated with active solar

regions. Pt. Ill covers relationships between radio emissions

from sun and solar disk features, and the origin of major bursts

and fading in enhanced radiation. The appendix describes the

D. T. M. solar radio interferometer. (Met. Abst. 7.5-148.)--

M.R.

D-598 Paetzold, H. K. and Zschomer, H. (both, Max-Planck-Inst.

fur Stratospharenphysik, Weissenau), Radiobeobachtunqen auf

20 MHz der ersten russischen Erdsatelliten. (Radio observations at 20 Mc/s of the first Russian satellite. ) TelefunkenZeitung, Berlin, 31(120):99-104, June 1958. 8 figs. , 5 refs.

French summary p. 99; English summary p. 104. DWB (629.

1388 P126ra) -Analysis of the Doppler effects of the 20 Mc/s

radio signals from the Sputniks I and II yielded the horizontal

structure of the ionosphere discussed here. The radio observations were conducted at the Institute of Stratospheric Physics,

213
»

Weissenau, Germany and the optical observations at the Telefunken Triangulation Laboratory* Ulm. The 2-3 min fadings

discussed in terms of the Cotton-Mouton effect and the Faraday effect indicate extension of ionospheric irregularities to

1000-2000 km. The existence of focusing elements, also

horizontally orientated over 100-200 km is plausible. A form

of "guidance" due to ionospheric refraction, rather than scattering, may enhance the 6000 km wave path. Excellent graphs

and reproductions of the original film recordings are given.

(Met. Abst. 11E-114.)»W. N.

D-59S Paetzold, H. K. , Die ersten kunstlichen Erdsatelliten. (Das

Internationale Geophysikalische Jahr, XIII). (The first artificial earth satellites (The International Geophysical Year, Pt.

13).) Die Umschau, Frankfurt a. M. , No. 1:3-7, 1958. 7

figs. DWB, DLC--Details of the first two Soviet satellites,

their trajectories, tracking and variations are discussed, along

with the first preliminary scientific results. It appears that

atmospheric density at 200-250 km is about double the value

assumed in the past. Radio signals are being received from

satellites far below the horizon which would indicate that

radio waves are channeled along the ionosphere for some time

before penetrating into the lower atmosphere. (Met. Abst.

10.7-92.)-G.T.

D-600 Paetzold, H. K. (Max-Planck-Inst. fur Aeronomie, Inst, fur

Stratospharen-Physik Weissenau, and Technische Hochschule

M&nchen), Einige Ergebnisse aus den Beobachtungen der

ersten russischen Erdsatelliten. (Some results of the observations of the first Russian artificial satellites. ) Raketentechnik und Raumfahrtforschung, Stuttgart, 2:50-54, April 1958.

7 figs. , table, 4 refs. , 8 eqs. DLC. Also his: Weitere Beobachtungen der russischen Erdsatelliten. (Further observations of the Russian earth satellites.) Ibid., 3(2) :45-49, April/

June 1959. 6 figs. , table, 14 refs. DLC, DWB (629. 1388

P126ei)--The orbits of the satellites 1957 Q~, and QLZ and &

and 1958 QCare tabulated and briefly discussed. The succeeding theoretical discussion of the state of the upper atmosphere

is based on visual and radio signal observations at different

locations in Germany. Some of the results are that (1) the density of air at very great heights is by far higher than assumed.

(2) The surface at immediate right angle to direction of movement rather than any aerodynamic effects of the shape of a satellite is what should be considered in quantitative evaluation.

(3) The impact of colliding air molecules with a satellite is as- sumed to be "elastic" (i. e., the former stick before thermally

evaporated). Ionospheric radio relationships are also touched

upon. The results are presented graphically. Further observations and measurements, especially with Sputnik III, have

been made since the first report on measurements with the first

214
Russian earth satellite one year ago. The radio signals of

this satellite have been received through 9 months. The re- sults described concern mainly the propagation of electromagnetic waves in the ionosphere and the structure of the upper

atmosphere. (Met. Abst. 11J-127.

)

Paetzold, H. K. (Max-Planck-Inst. of Aeronomy, Inst, fur

Stratospharen-Physik, Weissenau and T. H. Munchen), Observations of the Russian satellites and the structure of the outer

terrestrial atmosphere. Planetary and Space Science, N. Y. , 1(2):115-124, April 1959. 8 figs. , table, 24 refs. , 9 eqs.

DWB--The launching of the artificial earth satellites gave the

opportunity to gain some direct information about the outer re- gion of the earth's atmosphere. Our radio observations were

mostly made on 20 MHz with a new direction finder developed

by the firm Telefunken in Ulm. This instrument uses three

pairs of adcock antennas. The direction of the wave front and

the amplitude of the received signals can be measured at the

front of a television tube. A movie camera registers the pictures with a time resolution of 0. 1 sec. The accuracy of the

measured azimuths is about 0.5 . For 1957 OC , 1957/# and

1958 5 , optical observations of the German Moonwatch groups

were used. Further orbit data were obtained from the Moonwatch Headquarters, Cambridge, Mass. , the Air Force Cambridge Research Center, Bedford, Mass. , and the Vanguard

Computing Center, Washington. (Met. Abst. 11J-131. )--

Author's abstract.

//

Paetzold, H. K. and Zschorner, H. , Uber Dichteschwankunqen

der hcSchsten Atmosphare nach Satellitenmessunqen. (Density

variations of the highest atmosphere according to satellite measurements. ) 4 p. 3 figs. Reproduction of typescript (1959).

DWB (629. 1388 P126ub) -Observations of satellites Explorer V,

Sputnik III, and Vanguard I at the Telefunken Co. (20 Mc) and

elsewhere show that the density of the air during the day is 20%

higher than at night at 225 km, with extreme values in the evening and the morning, respectively, and the density also decreases from the high latitudes to the equator. Relation of density to solar activity, magnetic storms, solar UV, etc. , are also considered but not established, and data presented graphically to illustrate. (Met. Abst. 11J-130. )--M.R.

Paetzold, H. K. , Die oberste Erdatmosphare nach SatellitenMessunqen. (The upper atmosphere seen from satellite observations. ) Die Naturwissenschaften, Berlin, 46(13):416-422,

July 15, 1959. 7 figs. , 3 tables, 46 refs. DLC--With the aid

of artificial earth satellites, it is possible to study the ionosphere situated above the F2 peak level. In particular, the frequencies used in the Russian satellites (20 and 40 Mc/s) gave

interesting results according to which the electron density

215
seems to decrease slowly above the F2 layer. Fading observed

in the reception of these radio signals indicates the presence

of heterogeneities in the ionization, particularly in the polar

zones. For the explanation of a kind of periodic fading, it is

necessary to consider the rotation of the satellite and of the

antennas and also the influence of the geomagnetic field. Tern

perature and density values of the upper atmosphere can be deduced from the observation of the deceleration of artificial satellites. The temperature at 1000 km is in the range of 2000 K,

a value suitable to explain the escape of helium. Oscillations

of the value of the deceleration are associated with local var- iations of density and temperature. The discovery of the Van

Allen radiation belts, where particles are trapped in the geomagnetic field, is due to the cosmic ray equipment of earth satellites. The "Argus" experiment (explosion of A bombs at an

altitude of 500 km) showed the possibility of creating temporary radiation belts observed between the two natural belts by

satellites then in orbit. (Met. Abst. 11. 2-80. )--A. V.

D-604 Paetzold, H. K. (Max-Planck-Institut fur Aeronomie, Instut fur

StratOspharen-Physik, Weissenau and T. H. Munchen), Die

hochste Atmosphare und der Weltenraum. (The highest atmosphere and the cosmos. ) Umschau, Frankfurt a. M. , 59(l):3-6,

Jan. 1, 1959. 5 figs. , table. DLC--The audibility of the

Sputnik radio signals of 20 MHz and 40 MHz indicated that the

radio waves were refracted in the ionosphere; this is possible

only when the electron density does not fall below a value of

1. 10 electrons/cm in the maximum of the ionosphere at a height of 300 km. At greater altitudes the electron density

diminishes much more gradually than the atmospheric density.

The relative ionization gradually increases with altitude from

0. 05% at 300 km to 7% at 1000 km. From the Faraday frequency

perceptible in the satellite signals it was possible to compute

5 3

an electron density of 5. 10 electrons/cm at 500 km. The

temporary and irregular fading indicates the existence of ionospheric inhomogeneities. Duration of fading of several minutes

to several seconds indicated horizontal variations of electron

density extending from 2000 km to 100 km. The satellite became inaudible over higher latitudes at relative close distance

while from the south it was audible at great distances; this

indicates the influence of the polar ionosphere which is more

disturbed by incursion of corpuscle clouds than in lower latitudes. The shorter, life of the satellites as a result of deceleration indicates that atmospheric densities above 200 km are higher than hitherto expected. These higher densities signify

higher temperatures in the upper atmosphere. At 200, 350 and

1000 km the temperatures were 800, 2000 and 2500°K, respectively. The composition of theof; atmosphere comprises a density

*a of 100 nitrogen molecules/cm and 1 x 10 oxygen atoms/cm ,

216
and 0. 1% atomic hydrogen at about 80 km. At 1000 km there

are still 105 H-atoms/cm3

and at 3000 km 1000 H-atoms/cm3

may be present. At the high temperatures of the exosphere Hatoms are no longer stable but evaporate into the cosmos. Atmosphere density is greater by day than at night; variations

in density amounting to a factor of 10 result from a warming up

of the high atmosphere. The frequency of meteorites impinging

2

upon the satellite was 1 meteorite/100 m sec for meteorites

4 f^ in diameter; with increasing size the frequency diminished

by a factor of 10. The cosmic radiation was extraordinarily

high; at 1000 km it was 1000 times greater than the normal

cosmic radiation. The radiation particles were protons. The

maximum of radiation is apparently at 10, 000 km and above

this height it diminishes. The origin of the radiation belt is

discussed. (Met. Abst. 11J-129. )--I.L. D.

D-605 Paetzold, H. K. , Erforschung und Zustand der hochsten Atmosphere oberhalb der Ionosphere . (Exploration and state of the

highest atmosphere above the ionosphere. ) Reprint from Physikertagung Munchen, p. 63-82. Date not given. 13 figs.

,

5 tables, 24 refs. --The earth's atmosphere is bounded by the

earth's surface and by the interplanetary space with its very

slight mass density. The atmosphere is classified according

to its thermal state above the tropopause. A maximum is

reached in the mesosphere (280 K) at 45 to 50 km, but the ex- pected second maximum at 300-400 km is very probably not

reached because in this height the free path lengths of the

molecules and atoms are no longer small in comparison to the

extension of the atmosphere. The altitude at which this oc- curs is termed the critical height, which delimits the exosphere from the thermosphere. The author summarizes present

knowledge on the electron density and temperature in interplanetary space, the composition of the atmosphere and temperature distribution at the critical height, temperature, density, energy balance, disappearance of gases in the inner ex- osphere, and H-atoms in the outer exosphere and the use of

whistlers as a probe of the exosphere. (Met. Abst. 11. 8-179. ) -I.L.D.

D-606 Palmer, C. E. , Solar radio noise and high level zonal wind

shear over the central Pacific Ocean. Journal of Meteorology,

13(3):315-316, June 1956. fig. , 3 refs. DWB--A running plot

of zonal wind shear at 30, 000 ft between Wake Island and

Eniwetok Atoll shows that cyclonic shear reaches a maximum

8 days after a solar flare and anticyclonic shear 8 days after a quiet day. The index of solar activity is solar radio noise.

(Met. Abst. 7. 10-210. )-C.E. P. B.

217
D-607 Papaleksi, H. D. , Measurements of earth-moon distance by

means of electromagnetic waves. Elektrickestvo, (5):9-15,

1946. --The problem of pulse-echo method of time measurement

as applied in radar is analyzed thoroughly. The surface of the

moon is assumed to be of semireflecting nature. Lambert's

law is applied, and pulse forms after reflection from the moon

are calculated, based on three phases, the 1st phase being

contact of the leading edge of the pulse with the moon, and

2nd phase contact of the trailing edge with the moon, the 3rd

phase penetration of the centre of the moon. The importance

of beam angle, and the "illuminated" area are discussed. Minimum power for reliable reception is calculated for different frequencies, including light and zenith angle, and shown to be

practicable with power gains attained by modern aerial arrays

and pulse transmitters. The possibility of the use of light

waves (spark discharge) and the reception of the reflected

light signal by means of photocells is quantitatively discussed,

and a refinement proposed; the sending of pulses with distinct

spectral lines which should improve the signal/noise ratio of

reception. The feasibility of the experiment during a moon

eclipse (to exclude reflected sunlight) is stressed.

D-608 Paris Symposium on Radio Astronomy, July 30-Aug. 6, 1958,

(Proceedings) of Conference, July 30-Aug. 6, 1958. Ed. by

Ronald N. Bracewell. Stanford, California, Stanford Univ.

Press, 1959. 612 p. figs., tables, refs. , eqs. Price: $15. 00.

(International Astronomical Union, Symposium, No. 9 and International Scientific Radio Union, Symposium No. 1). DLC

(QB475. P26)--Some of the 107 papers in the Proceedings are included in the present bibliography under the individual authors. (All will be abstracted in Meteorological and Geoastrophysical Abstracts). However, for the reader's convenience,

all of the 107 papers are listed below in alphabetical order by

the authors names, indexed individually under the corporate

reference No. D-608. Adgie, R.L. : An attempt to detect the

327 Mc/s line of galactic deuterium, p. 352-354. Alekseev, U.

and Vitkevich, V. V. : On the polarization of radio emission at

1. 5 m wavelength, p. 259-262. Alsop, L. E. ; Giordmaine, J. A.;

Mayer, C.H. and Townes, C.H. : Observations of discrete

sources at 3 cm wavelength using a maser, p. 69-74. Archer, S.;

Baldwin, J. R. ; Edge, D. O. et al. : Studies of radio sources at

159 Mc/s, p. 487-491. Athay, R. G. : A model of the chromos - phere from radio and optical data, p. 98-104. Avignon, Yvette;

Boischot, A. and Simon, P. : Observation interferometrique a 169 Mc/s des centres R. sources des oraqes de bruit, (Interferometric observation at 169 Mc/s from R centers, source of

noise storms), p. 240-244. Baldwin, J. E. and Shakeshaft, J.R.:

Radio emission from the direction of the super galaxy, p. 347-

351. Baldwin, J. E. : Galactic background surveys and the galactic halo, p. 460-464. Basinski, Jane; Bok, B. J. and

218
Gottlieb, K. : Optical identification of southern radio sources.

p. 514-522. Blaauw, Z. : The large scale structure of galaxies: concluding lecture, p. 466-468. Blum, E. J. and Boischot,

A. : Eclipse de la nebuleuse du Crabe par la couronne solaire,

(Eclipse of the Crab nebula by the solar corona), p. 282-285.

Boischot, A. and Simon, P. : La composante leatement variable

du rayonnement solaire' sur 169 Mc/s, (Variable slow component of the sun's radiation on 169 Mc/s), p. 140-142. Boischot,

A. : Les emissions de type IV, (Type IV emissions), p. 186-

187. Boischot, A. and Fokker, A. D. : The 1957 Nov. 4 event.

p. 263-267. Boischot, A. : Resultats preliminaires de 1' obser- vation des radiosources a l'aide de l'interferometre de Nancay,

(Preliminary results of the observation of radio sources using

the Nancay interferometer), p. 492-495. Brown, R.Hanbury;

The distribution and identification of the sources, p. 471-474.

Burbidge, E. Margaret and Burbidge, G. R. : The radio source

in the Cygnus loop and IC443, p. 323-327. Burbidge, G. R. : The theoretical explanation of radio emission, p. 541-551.

Burke, B. F. ; Ecklund, E. T. ; Firor, J. W. et al. : Atomic hydro- gen survey near the galactic plane, p. 374-389. Christiansen,

W. N. and Mathewson, D. S. : The origin of the slowly varying

component, p. 108-117. Cohen, M.H. and Fokkes, A. D. : Some remarks on the polarization of 200 Mc/s polar radio emission, p. 252-258. Covington, A. E. : Solar emission at 10 cm

wavelength, p. 159-165. Davies, R. D. : Substructure within

galactic spiral arms as derived from studies at 21 cm, p. 355-

359. de Groot, T. : Spectra of short lived transients in solar

noise at 400 Mc/s. p. 245-247. de Jager, C. : The structure

of the chromosphere and the low corona , p. 89-97. Denisse,

J. F. : Les sources d'emissions radioelectriques du soleil, (The

sources of radioelectric emissions of the sun), p. 81-88.

Denisse, J. F. : Relation entre les emissions de rayons cosmiques solaires et certains sursauts radioelectriques, (Relation between solar cosmic ray emissions and certain radioelectric bursts), p. 237-239. Dewhirst, D. W. : The optical identification of radio sources, p. 507-513. Drake, F. D. : The nature

of the radio source Cygnus X, p. 339-346. Drake, F. D. : Neutral hydrogen in galactic clusters, p. 366-369. Elgaroy, O. : Frequency drift and flat structure of 200 Mc/s solar bursts,

p. 248-250. Elsmore, B. : Radio observations of the lunar atmosphere, p. 47-49. Elsmore, B. : The accurate positions of

17 intense radio sources, p. 337-338. Erickson, W. C. ; Heifer,

H.L. and Tatel, H. E. : A survey of neutral hydrogen at high

galactic latitudes, p. 390-397. Evans, J. V. ; Evans, S. and

Thomson, J. H. : Rapid fading of moon echoes at 100 Mc/s.

p. 8-12. Firor, J. : The quiet sun at 88 cm wavelength, p. 107.

Firor, J. : Solar radio bright spots at 88 cm wavelength, p. 136-

139. Fleischer, R. : Variations in 18 Mc/s solar and cosmic

noise, p. 208-209. Gelfreich, G. ; Korol'kov, D. ; Rishkov,

N. and Soboleva, N. S. : On the regions over sunspots as

219
studied by polarization observations on centimeter wavelengths, p. 125-128. Gelfreich, G.B. ; Ikhsanova, V. N. ; Kaldanovskii, N. L. et al. : Bursts of microwave radio emission associated with solar flare, p. 218-221. Gibson, J. £. and McEwan,

R.J. : Observations of Venus at 8. 6 mm wavelength, p. 50-52.

Ginzburg, V.L. : On the mechanisms of sporadic solar radio

emission, p. 574-582. Ginzburg, V.L. : Radio astronomy and

the origin of cosmic rays, p. 589-594. Giovanelli, R. G. and

Roberts, J. A.-: Optical observations of solar disturbances

causing type II radio bursts, p. 201-202. Giovanelli, R. G.

Flare puffs as a cause of type HI radio bursts, p. 214. Gold, T.

Cosmic rays and radio waves as manifestations of a hot uni- verse, p. 583-588. Gutmann, Monique and Steinberg, J. L.

Resultats preliminaires obtenus avec l'lnterferometre a 8 an- tennes sur 3 cm de longueur d'onde. (Preliminary results with

an 8 antennae interferometer on 3 cm wavelength), p. 123-124.

Haddock, F. T. : Some characteristics of dynamic spectra of

solar bursts, p. 183-193. Hartz, T. R. : Radio noise measurements on the passage of solar particles through the corona.

p. 554-561. Hazard, C. and Walsh, D. : A comparison of an

interferometer and total power survey of discrete sources of

radio frequency radiation, p. 477-486. Hewish, A. : The scattering of radio waves in the solar corona, p. 268-273. Hey,

J. S. and Hughes, V.A. : Radar observations of the moon at

10 cm wavelength, p. 13-18. Hey, J. S. : The first discovery

of point sources, p. 295-296. Hogbom, J. A. : The instantaneous position and diameter of short duration bursts of solar

radio emission, p. 251. Hoyle, F. : The relation of radio astronomy to cosmology, p. 529-532. Hoyle, F. : Mechanisms of

solar and cosmic emission: concluding lecture, p. 598-601.

Ikhsanova, V. : Solar observations with the large Pulkovo radio

telescope at 3. 2 cm wavelength, p. 171-173. Jennison, R.C.:

The structure of the Cassiopeia A and Cygnus A radio sources

measured at 127 Mc/s and 3000 Mc/s, p. 309-314. Khalkin,

S. E. and Kaidanovskii, N. L. : A new radio telescope of high

resolving power, p. 166-170. Kundu, M. R. : Etude interferometrigue des sources d'activite solaire sur 3 cm de longueur

d'onde. (Interferometric study of sources of solar activity on

3 cm wavelength), p. 222-236. Kuz'min, A. D. and Udal'tsov,

V. A. : Polarization of 10 cm radiation of the Crab nebula,p. SOSSOS. Link, Frantisek: Sur les ionospheres pianetaires. (Planetary ionospheres), p. 58-60. Link, Frantisek: Manifestations

possibles de la couronne de Chapman dans la radio astronomie.

(Possible manifestations of the Chapman corona in radio astronomy), p. 274. Lovell, A. C.B. : Moon and planets: concluding

lecture, p. 75-78. McClain, E. F. and Sloanaker, R. M. : Preliminary observations at 10 cm wavelength using the NRL 84 ft radio telescope, p. 61-68. McVittie, G. C. : Remarks on cosmology, p. 533-535. Mills, B. Y. : Galactic structure at meter

wavelengths, p. 431-446. Mills, B. Y. : A survey of radio

220
sources at 3. 5 m wavelength, p. 498-506. Minkowski, R. : Optical observations of nonthermal galactic radio sources f p. 315-322. Minkowski, R. : Discrete sources and the uni - verse: concluding lecture, p. 536-538. Minnaert, M. G. J.

The sun: concluding lecture, p. 286-292. Molchanov, A. P. ; Chen, Fan-Yun; Wang, Shou-Kuang et al. : Preliminary re- sults of radio astronomical observations of annular solar

eclipse. April 19. 1958. p. 174-175. Muller, C.A. : 21 cm

hydrogen line absorption in the spectra of discrete sources.

p. 360-365. Muller, C. A. : Hydrogen line observations on

the coma cluster, p. 465. Newkirk, G. , Jr. : A model of the

electron corona with reference to radio observations, p. 149-

158. Oort, J. H. : A summary and assessment of current 21-

cm results concerning spiral and disk structures in our galaxy,

p. 409-415. Panovkin, B. N. : A model of the inner corona

based on radio data, p. 105-106. Pawsey, J. L. : Radio evidence on the large scale structure of our own and external

galaxies, p. 405-408, Roberts, J. A. : Some aspects of type

II bursts, p. 194-200. Rougoor, G. W. and Oort, J. H. : Neutral hydrogen in the central part of the galactic system, p. 416-

422. Ryle, M. : The problem of confusion in surveys of

sources, p. 475-4/ C. Ryle, M. : The nature of the radio

sources, p. 523-528. Sanamian, V. A. and Tovmasian, H. M. : On increase of the sensitivity and directivity of radio interferometers, p. 496-497. Schatzman, E. : On the possibility of

observing radio emission from flare stars, p. 552-553. Senior,

T. B. A. and Siegel, K. M. : Radar reflection characteristics of

the moon, p. 29-46. Shain, C. A. : Observations of extragalactic radio emission, p. 328-336. Shain, C. A. : Absorption of

19. 7 Mc/s in H II regions, p. 451-459. Smith, F. G. : Radio

astronomy and the solar system, p. 3-7. Smith, Harlan J. and

Douglas, J. N. : Observations of planetary nonthermal radiation, p. 53-55. Takakura, T. : Synchrotron radiation and solar

radio outbursts at microwave frequencies, p. 562-570. Tanaka,

H. and Kakinuma, T. : Polarization of bursts of solar radio

emission at microwave frequencies, p. 215-217. Thompson,

A. R. : The correlation of solar radio bursts with magnetic activity and cosmic ravs. p. 210-213. Tunmer, Harriet: The origin of the belt of galactic radio waves, p. 571-573. van de

Hulst, H. C. : Galactic and extragalactic radio sources: concluding lecture, p. 398-401. Van Woerden, H. : The distribution of neutral hydrogen in the Orion region, p. 370-373. Vauquois, B. : Etude statistique de la composante lentement variable d'apres les observations entre 10. 000 et 600 Mc/s. (Statistical study of the variable slow component according to observations between 10, 000 and 600 Mc/s), p. 143-148. Vitkevich, V. V. ; Kuz'min, A. D. ; Salomonovich, A. E. and Udal'tsov, V. A. : Radio picture of the sun at 3. 2 cm wavelength.

p. 129-135. Vitkevich, V. V. : New data on the solar supercorona, p. 275-281. Volders, Louise and van de Hulst, H. C. :

221
Neutral hydrogen in extragalactic systems, p. 423-430.

Waldmeier, M. : A comparison between radiohelioqrams and

optical observations of the solar corona, p. 118-122. Wallis,

G. : The determination of the energy distribution of relativistic

electrons by the frequency distribution of their "synchrotron

radiation" , p. 595-597. Warwick, Constance and Warwick,

J. W. : Flare associated bursts at 18 Mc/s, p. 203-207. Westerhout, G. : 75 cm and 22 cm continuum surveys, p. 447-450.

Whitfield, G. R. and Hogbom, J. : Radio observations of the

comet Arend-Roland. p. 56-57. Whitfield, G. R. : The spectra

of radio sources, p. 297-304. Wild, J. P. ; Sheridan, K. V. and

Trent, G. H. : The transverse motions of the sources of solar

radio bursts, p. 176-186. Yaplee, B. S. ; Roman, Nancy G. ; Craig, K. J. and Sc anion, T. F. : A lunar radar study at 10 cm

wavelength, p. 19-28. --W. N.

D-609 Patterson, T. N.L. (Queen's Univ. of Belfast, Ireland), Whistler dispersions for a model of the ionic distribution in the exosphere. Planetary and Space Science, N. Y. , 8(2):71-76, Nov.

1961. 2 figs. , 3 tables, 3 refs. , 16 eqs. DWB--Calculations

are presented of the dispersions of whistling atmospherics for a model of the ion distributions in the exosphere. Exospheric

temperatures of 1000°!^ 1250°K,

o

1500°K and 2000°K are considered at latitudes 30 , 35 , 40 , and 45 and corresponding

to various transition levels at which n (500 km ) equals

n(500 km H ). Comparison is made with two observed whistlers. (Met. Abst. unpub. ) --Author's abstract.

D-610 Pawsey, J. L. ; McCready, L. L. and Gardner, F. F. , Ionospheric thermal radiation at radio frequencies. Pt. 1. Journal of

Atmospheric and Terrestrial Physics, l(5/6):261-277, 1951. 9

figs. , 2 tables, 6 refs. Also: Gardner, F. F. , Pt. 2.

Further observations. Ibid. , 5(5/6) :298-315, 1954. 11 figs.

,

2 tables, 10 refs. , eq. DWB--Part 1 - Minimizing man made

radio noises and atmospherics - the thermal radiation from the

ionosphere has been identified and measured. The electron

temperature at 70-80 km was found to be 240-290°K. Pt. 2 - Radio noise on 2 Mc/s at Urisiono (30 S 144 a) a very quiet

site in Australia, is attributed almost entirely to ionospheric

thermal radiation. Temperatures (200-250 K ) show no diurnal

variation but vary greatly from day to day especially in summer,

and increase by up to 40 K on SID days. Polarization measurements in Sept. 1951 showed that the extraordinary component

was absorbed at a lower level 20 K warmer than ordinary component, indicating that temperature decreases with height. Messurements fit temperature height model given by rockets but

about 40 K warmer, giving minimum of 217 K at 80 km. Some

observations of noise of tropospheric origin are described.

(Met. Abst. 12E-72.)-A.A. andC.E.P.B.

222
Pawsey, J. L. , A catalogue of reliably known discrete sources

of cosmic radio waves. Astrophysical Journal, Chicago, 121

(l):l-5, Jan. 1955. 3 tables, 21 refs. DWB--As a part of the

work of Commission 40 of the International Astronomical Union,

a list of reliably known discrete sources of cosmic radio waves

has been prepared by a committee consisting of J.G.BOLTON,

R. HANBURY BROWN, F„ G„ SMITH and B. Y. MILLS. In this

paper this list is published, with a short description of the

catalogue by the president of the commission, Jo Lo PAWSEY.

(Met. Abst. 9A-86. )--Author's abstract.

Pawsey, J. L. and Bracewell, R. N. , Radio astronomy. Oxford,

Clarendon Press, 1955. 361 p. 150 figs. , 23 tables, 23

plates. Bibliog. at end of each ch. Price: 55 sh. (International Monographs on Radio) DLC (QB475.P3). Review by

P. ten Bruggencate in Die Naturwissenschaften, Berlin, 44(17):

476, Sept. 1, 1957. --This substantial textbook covers the history of radioastronomy, techniques for observation of extraterrestrial radio waves, theory of radio waves in ionized gases,

solar physics, solar radio waves, astrophysics, cosmic radio

waves, thermal radio waves from moon, extraterrestrial radio

echoes, meteors, and effects of terrestrial atmosphere on extraterrestrial radio waves. The work is well indexed, excellently illustrated and contains good referencing lists at the end

of each chapter. The last chapter discusses effects of the lower and upper atmosphere and ionosphere on absorption and

twinkling of radio stars. (Met. Abst. 9A-87. )--M. R.

Pawsey, J. L. , The question of radio emission by the ionosphere. Journal of Atmospheric and Terrestrial Physics, London,

15(1/2): 51 -53, Sept. 1959. 10 refs. DLC--The importance of

non-thermal emission of radio waves of the ionosphere as a probable source of "radio noise from the aurora** in ionospheric

and astronomical studies is examined. The thermal emission

from the D region does not preclude occasional bursts nor intense emission from the £ layer. Intense noise from all over

the sky reported on meter wavelengths, and other similar re- ports, until reliably reproduced, present clues rather than evidence. Brief increases of noise level on a frequency of 33

Mc/s coinciding with meteors might originate from a source

other than the meteor. GALLET's report giving reasons for supposing the "dawn chorus" is generated in the outer reaches of

the ionosphere, is worthy of further examination. (Met. Abst.

11. 12-323. )--O.T.

Pecker, Jean-Claude, Activite solaire et maqnetisme terrestre.

(Solar activity and earth's magnetism. ) L'Astronomie, Paris,

72(12):485-498, Dec. 1958. 10 figs. , 5 refs. DWB- The un- steady part of the earth's magnetic field is principally due to

the electromagnetic activity of the very high atmosphere which

223
is the most sensitive to solar influences. The first part concerns the sun: description of the outer layers of the sun,

commentaries on solar activity, research and study of solar

influences on terrestrial phenomena. The second part deals

with variations of the earth's magnetism: methods of study,

influences on the geomagnetic indexes, association of solar

phenomena with recurrent geomagnetic activity and theory of

the geomagnetism of corpuscular origin. The study of geomagnetism can supply valuable data about ionosphere and

propagation of radioelectric waves. Another application of

the study of geomagnetism is to meteorology, for solar influence on the terrestrial atmosphere appears to be evident.

(Met. Abst. 11. 2-164. )-A.V.

D-615 Penico, A. J. , Propagation of electromagnetic waves in a

plasma with inhomogeneous electron density. Planetary and

Space Science, N. Y. , 6:222, June 1961. Abstract only.

The paper was presented at the Plasma Sheath Symposium,

Boston, Mass., Dec. 7-9, 1959.—A theoretical study was

performed to determine the propagation characteristics of 'an

electromagnetic wave in the presence of an isotropic, dissipative plasma whose electron density varies in the direction

of propagation of the wave. In the analysis, various functional forms giving the electron density as a function of the

position within the plasma were inserted into the v/ave equation for the medium, and exact solutions were obtained for

the equation. The above mentioned solutions will be discussed from two points of view. First, their qualitative behavior for all, or nearly all, of the values of the parameters

will be discussed. Second, curves will be shown indicating

the specific behavior of the solutions for limited ranges of

radio frequency, electron-neutral particle collision frequency,

initial and final electron density and rate of variation of the

electron density. Criteria will be discussed for treating the

electron density as "slowly varying" or "rapidly varying." In

particular, some "quarter wavelength" and "half wavelength"

criteria of the medium will be exhibited. These criteria will

be discussed in relation to the problems of reflection and

absorption of the waves.

D-616 Perlman, S. ; Kelly, L. C. ; Russel, W. J. and Stuart, W. D.,

Concerning optimum frequencies for space vehicle communica- tion. Institute of Radio Engineers. Professional Group of

Communications Systems, New York, Transactions, Vol. CS7(3):167-173, Sept. 1959. 9 figs. , 11 refs. , 7 eqs. DLC--

This is a condensed form of the U. S. Army Signal Radio Propagation Agency's report entitled 'Tentative evaluation of the

transmission factors for space vehicle communication. " Equipment factors, propagation factors, auroral effects, absorption, polarization, radio star scintillation and noise are

224
discussed. A 12 db improvement in receiver sensitivity re- presents these choices: (1) Four-time increase of space communication; (2) 1/16 transmission power for same distance

of communication; (3) Less directive antenna with up to 12

db less gain, or a combination of any two or three factors.

--W. N.

D-617 Peterson, A. M. et al. (all, Stanford Research Inst. , Menlo

Park, Calif. ), Radio and radar tracking of the Russian earth

satellite. Institute of Radio Engineers, N. Y. , Proceedings,

45(11): 1553-1555, Nov. 1957. 5 figs. , table. DLC--Brief

account of techniques employed and results obtained at the

Stanford Research Institute. Experimental measurements

with hastily assembled equipment — now improved — appear

to yield valuable scientific data on the upper atmosphere.

(Met. Abst. 9.8-51.)--W.N.

D-618 Peterson, L. E. and Winekler, J. R. (both, School of Physics,

Univ. Minn. , Minneapolis), Gamma-ray burst from a solar

flare. Journal of Geophysical Research, Wash., D. C.,64(7):

697-707, July 1959. 7 figs. , 3 tables, 16 refs. DLC--A

burst of high energy radiation coincident with a solar flare

has been detected during a balloon flight at 10 gm/cm^ atmosphere depth and 30 geomagnetic latitude over Cuba. The

flare occurred at 1305 UT on March 20, 1958 and was associated with solar radio bursts on 1, 500 and 10, 000 Mc/s.

Terrestrial effects included a SID, earth current disturbance,

and a magnetic crotchet. The 18 sec burst was detected

with an integrating ionization chamber and a single Geiger

counter. From these two instruments and their ratio, it is

inferred that the radiation is due to a gamma ray flux of

-5 2

about 2 X 10 ergs/sec cm peaked in the 200 to 500 Kv re- gion. This radiation can be interpreted as bremsstrahlung

produced in the solar photosphere from electrons of 0. 5 to

1 Mev energy. These same electrons, spiraling in a 1000

gauss field in the flare region, can produce the observed

radio burst by betatron radiation. The high energy electrons

represent about 1% of the flare energy. Only about 0. 01% of

the emitted betatron radiation escaped from the flare region

toward the earth. (Met. Abst. 11. 9-72. )—Authors abstract.

D-619 Petri, Winfried (Schliersee Obs. ), Auf der Schwelle des

Weltraums: bericht fiber die ersten Wochen der kunstlichen

Erdsatelliten (Sputniki) 1957 <W . OC2xmd 6 . (At the threshold of outer space: Report on the first week of artificial

earth satellites (Sputniks) 1957 0L± , <t z and £ . ) Naturwissenschaftliche Rundschau, Stuttgart, 11(1): 1-7, Jan. 1958.

7 figs. , 5 tables, eqs. DWB, DLC--The author summarizes

Soviet studies on experimental rockets appearing in the Soviet

225
M

literature prior to the launching of Sputnik I and II, including

description of the structure of the rockets, indication of satellite launching and various information on the instrumentation for obtaining data on outer space and on the duration of

the recording and transmission time. This is followed by a discussion of the celestial mechanics of satellites close to

the earth, the influence of gravity upon the satellite path,

the effect of precession upon the rotation of the plane of the

path, the rotation of the opsidal lines, the braking action of

atmospheric density upon the path, etc. ; the visual observation methods employed to track the satellite, namely: "moonwatch"; various problems in determining the time of revolution of the satellite by visual means; reception of signals

from the satellite radio by "Minitrack"; the radio interferometer technique; evaluation of the radio signals and lunar

echoes from the Sputnik. Diagrams showing the motion of

Sputnik within 24 hrs, a comparison of the paths of the first

two satellites, and graphs showing the variation of atmospheric pressure with altitude according to Soviet data, U. S.

data and the standard atmosphere, satellite path at 530 km,

variation of reception frequency as a function of time, and

variation in the revolution period of satellite CCz. and numerical data on the first two satellites. (Met. Abst. 11J-133.

)

-I.L.D.

D-620 Petri, W. (Schliersee/Obb. ) and Faust, H. (Offenbach),

Neue Satelliten-Erqebnisse. (New satellite findings.) Naturwissenschaftliche Rundschau, Stuttgart, 11(12):460-461, Dec.

1958. fig. DWB, DLC--There are four brief notes entitled:

(1) Density variation of the upper atmosphere. G.HERGNHAHN discovered that the orbital period of Sputnik 2 and

Sputnik 3 decreased (up to 40%) rather than increased. The

discovery was made while analyzing the Doppler effects of

the satellite borne radios. The phenomenon may be due to a drop of 25 km of the atmosphere, or less plausible, less air

friction due to self orientation of the cone shaped satellite

exposing least resistance surface. (2) Micrometeorites. The

10 kg Vanguard, fired May 27, 1958, reached about 3000 km

altitude and was hit by 17 micrometeorites during ten minutes.

Assuming that these figures are representative, the earth is

bombarded at least five times heavier than was believed. (3)

Contour of the earth. U. S. 1958 Alpha and Beta 2 satellite

observations show that the earth is not as flat as assumed.

The difference is 200 m in favor of the polar diameter vs. the

equatorial. The observations of U. S. S. R. satellite, 1957

Beta, made by the English Air Force Research Establishment

at Farnborough, found the earth oblateness to be 1/298. 1

rather than 1/297. 1. (4) State of the upper atmospheric lay- ers on bases of satellite measurements. PAETZOLD's remarkable results showing a very active dynamic of the upper

226
atmosphere were arrived at with the aid of Sputnik 1 and

Sputnik 3. Electron density, ionization, air density and

temperatures are briefly discussed. The density of air at

225 km altitude above the equator is only half of the density

of the air above the pole. The density and temperature decline from the pole toward the equator is associated with

strong E-W winds. (Met. Abst. 11J-134. )--W. N.

D-621 Petri, W. , Unbekannte Hcftienstrahlunq hSher Intensitat.

(Unknown high altitude radiation of great intensity.) Naturwissenschaftliche Rundschau, Stuttgart, 11(7): 274, July 1958.

DWB, DLC--According to J. van Allen the satellite "Explorer"

recorded at 1500 km an increase in ionospheric radiation that

was more than a thousandfold that recorded at an altitude of

400 km. It corresponded to an equivalent of 0. 06 Rontgen

per hour, and it was so strong that the geiger counter could

not operate. It is possible that this is a hard X-ray radiation

which is produced by the action of the solar particles upon

the residual atmosphere or upon the body of the satellite. If

this radiation is the result of an interaction between the particles with extensions of the earth's atmosphere it may disappear at a distance of 2-3 earth radii. --I.L.D.

D-622 Pettengill, Gordon, H. (Lincoln Lab. , M. I. T. , Lexington,

Mass.), Measurements of lunar reflectivity using the Millstone Radar. Institute of Radic Engineers, N. Y. , Proceedings, 48(5): 933-934, May 1960. 3 figs. , table, 7 refs. DLC

--Successful results of lunar mapping conducted at Lincoln

Laboratory, M. I. T. , with a new method for mapping radar

echo sources from remote rotating targets, are discussed

briefly. The method renders accurate frequency data without sacrifice in range solution. Thus, a precision of approximately 0. 02 in 10° of the observed Doppler frequency

during low libration periods is feasible. Lunar range frequency contours and processed results of a run near maximum

libration are given along with tabulated radar parameters.

»W. N.

D-623 Pfeiffer, John, The changing universe: the story of the new

astronomy. New York, Random House, 1956. 243 p. numerous illus. DLC. Review by F. G. Smith in Nature, London,

181(4614) :980, April 5, 1958. Review by A. J. M. Wanders in

Hemel en Dampkring, The Hague, 56(11):217-218, Nov. 1958.

—The exciting story of radio astronomy from the accidental

discovery which led to its birth in New Jersey in 1931-33 (by

KARL JANSKY) and development during 1938-44 (by GROTE

REBER) in Illinois, and its post war development in England

and Australia up to the building of the huge radio telescopes

and even larger ones proposed in the last few years. Radio

waves from Orion, the Galaxy, the solar system, the sun,

227
constellations from beyond the Milky Way, Belts of Galaxies, source of energy, hydrogen sources, obscuring dust,

birth of stars, spiral arms, meteor flares, the moon, atmospheric absorption and transmission, twinkling radio stars,

relation of radio stars to atomic power, are described in a

lively manner by a thoroughgoing science reporter in this

book. (Met. Abst. 11. 7-20. )--M. R.

D-624 Pfister, Wolfgang (Ionospheric Physics Lab. , Geophysics

Res. Directorate, A. F. Cambridge Res. Center), Study of

fine structure and irregularities of the ionosphere with rockets and satellites. (In: Van Allen, James A. (ed. ), Scientific uses of earth satellites . Ann Arbor, Univ. of Michigan

Press, 1956. p. 283-291. 2 figs.) DWB, DLC-Almost all

experiments using the ionosphere as a propagation medium

reveal the presence of irregular or blobby structure in the

electron distribution, and, consequently, a variety of methods is in use to determine something about the blobby structure, either by propagation through the ionosphere as in the

radioastronomic technique or by reflection within the layers.

Only limited information is available from rocket experiments,

but due to the fact that a rocket or satellite travels in the

midst of the ionosphere, experiments using transmissions between the vehicle and the ground will be able to add a new

and very valuable type of information. Up to now, the contribution of the irregularities has been looked at more as a

nasty by-product which must be smoothed out in the data

analysis. However, from the data available, an analysis in

terms of irregular structure appears to be quite promising.

Based on experience with known techniques, a set of experiments for a satellite is being proposed. It is a combination

of the pulse delay experiment similar to the Air Force electron density rocket experiment with a kind of drift type ex- periment measuring the signal amplitude fluctuations at three

closely spaced receivers. The real advantage of the fine

structure experiment with satellites or rockets will be that

the changing aspect allows us to gain a three-dimensional

picture of the configuration of the blob, while so far we are used to looking only at the two dimensional diffraction pattern at the ground. (Met. Abst. 9. 3-83. )- -Author's abstract.

D-625 Pfister, W. and Keneshea, T. J. , Ionospheric effects on

positioning of vehicles at high altitudes . U. S. Air Force.

Cambridge Research Center. Air Force Surveys in Geophysics, No. 83, March 1956. 27 + p. numerous figs. , table,

7 refs. , numerous eqs. DWB, DLC—When a radio wave penetrates the ionospheric region, the presence of free electrons

there causes it to deviate from its straight line path. The

predictable part of this effect has been computed in terms of error in the initial angle of propagation and the error in the

228
range of points in the ionized region. The results are contained in a series of graphs. The maximum error for a frequency

of! 1000 Mc/s is of the order of 0. 1 mil and 45 meters, ' respectively; these values being inversely proportional to

the frequency. The unpredictable part of the effects of the

ionosphere is randomly varying and unknown in its details,

especially the dependence on frequency. From known facts

of the ionospheric irregularities and from theoretical considerations a justifiable estimate of the effects can be obtained.

This estimate is based on the angular spread and other quantities derived from ionospheric drift measurements and on an

experimentally confirmed frequency dependence law. (Met.

Abst. 11E-115. )--Authors' abstract.

Pfister, W. and Ulwick, J. C. (both, A. F. Cambridge Res.

Center, Bedford, Mass. ), The analysis of rocket experiments

in terms of electron density distributions. Journal of Geophysical Research, Wash., D. C, 63(2):315-333, June 1958. 14

figs. , table, 10 refs. DLC --Rocket ionosphere experiments

give the relative delay of a pulsed signal as a function of rocket position. These data are used in an analysis to obtain the

electron density distribution with respect to height. This an- alysis, which takes into account the effects of the earth's

magnetic field and the obliquity of the ray paths, is for the

smooth, horizontally stratified ionosphere. The actual ionosphere, however, has an irregular or "blobby" structure evident

in our delay records. The data then must be smoothed over a height interval corresponding roughly to the size of the blobs.

The delay data from U. S. A. F. Aerobee No. y%, which was

launched at 1210 hrs MST on June 26, 1953, at Holloman Air

Development Center, New Mexico, are analyzed for rocket as- cent and descent for two frequencies, 4. 05 and 4. 87 Mc. The

electron density distribution from rocket descent data for both

frequencies are in good agreement and show peaks at 106, 111,

117, and 128 km. For rocket ascent, an intense irregularity

apparently was present around 98 km, with a minimum horizontal extension of 3. 5 km and a maximum intensity of about

4 3 6 X 10 electrons/cm . The P'-f record taken at launch time

compares very well with the electron density distribution from

rocket descent. (Met. Abst. 10. 3-205. )--Authors' abstract.

Pick-Gutmann, Monique, Sur la structure des types IV: les

orages continuum. (The structure of type IV jumps: the continuum storms. ) Academie des Sciences, Paris, Comptes

Rendus, 250(12): 2127-2129, March 21, 1960. 2 figs. , 7 refs.

DWB, DLC --One distinguishes two phases in the evolution of

the type IV jumps. In the first phase, the duration of which

seldom exceeds a quarter of an hour, the continuous radiation

always occurs on centimeter or decimeter waves. In the sec- ond phase, the continuum occurs essentially on meter waves;

229
«»^

this emission may last from some tens of minutes to 1 or 2

days in exceptional cases. This second phase resembles

radioelectric storms by both its duration and its spectrum.

The 24 hr continuums present a set of characteristics which

seem to define a class of distinct phenomena called by the

author continuum storms. These are always preceded by a very important chromospheric eruption and by a very intense

first phase. It is difficult to specify whether the continuum

storm is to be considered as a transformation of the first

phase of the type IV jump or as an independent phenomenon

linked also with the chromospheric eruption. (Met. Abst.

11. 12-56. )--A.V.

D-628 Piddington, J. H. and Minnett, H. C. , Solar radio frequency

emission from localized regions at very high temperatures.

Australian Journal of Scientific Research, Ser. A, Physical

Sciences, 4(2):131-157, June 1951. 11 figs. , 5 tables, refs.,

6 eqs. MH-BH--Solar radio frequency radiation is analyzed

into three components: a basic steady component B, a slowly varying component S, and various forms of more or less

rapid fluctuations called the X component. The spectra of

all three components are drawn between 600 and 24, 000 Mc/s,

and suggested extensions to lower frequencies are discussed.

The properties of the S component are described in some detail; these include correlation with sunspot data, polarization, and the location of the sources of origin. Evidence is

presented in favor of generation by thermal processes. It is

suggested that the S component is due to thermal emission

from localized regions at temperatures of about 10^ K, often

in the vicinity of sunspot s. The radiation from a model hot

region is examined in detail and the emission spectrum and

polarization characteristics are derived. The results are found to compare reasonably with observation. Thermonic

emission of electrons and protons would probably occur from

the hot regions. These particles would travel to the earth

with average velocities of a few hundred kilometers per sec

and may be identical with the slow corpuscular radiation

whose presence is deduced from terrestrial magnetic data.

(Met. Abst. 4.9-109.) -Authors' abstract.

D-629 Piddington, J. H. and Minnett, H. C. , Observations of galac - tic radiation at frequencies of 1210 and 3000 Mc/s. Australian

Journal of Scientific Research, Ser. A, Physical Sciences,

4(4):459-475, Dec. 1951. 6 figs. , table, refs. MH-BH--

Measurements are described of galactic radiation of 1210 and

3000 Mc/s. The results provide extensions of previous radio

emission spectra by more than 1& octaves. The intensity of

radiation from near the galactic center was measured and an

estimate made of the direction of the maximum of such radiation. A new "discrete source" of peculiar spectrum was

230
discovered very close to the center of the Galaxy. Evidence

suggests that the power output of this and some other sources

in the radio spectrum may exceed the total output of the sun. Radiation was also observed from the direction of the Crab

Nebula, from the known "radio source" in Centaurus, and from

the moon. Two nebulae (M 31 and NGC 7293) were investigated with negative results. The spectra of two sources are given between the limits 18. 3 and 1200 Mc/s. (Met. Abst.

4. 9-114. )--Authors' abstract.

D-630 Piddington, J. H. , Thermal theories of the high intensity com- ponents of solar radio frequency radiation. Physical Society

of London, Proceedings, Ser. B, 66(2):97-104, Feb. 1, 1953.

18 refs. DLC--Thermal brightness of solar radio frequency

radiation reaches 10 - 10 K in "noise storms" and outbursts, often with maximum near 100 Mc/s. Thermal theories

of origin are discussed and rejected. It is considered that

high intensity components of solar and galactic radiation

must be due, at least in part, to ordered non-thermal motion

of electrons. (Met. Abst. 4. 9-108. )--C. E. P. B.

D-631 Piggott, W. R. , D. S. I. R. ionospheric absorption measuring

equipment. Wireless Engineer, London, 32(6): 164-169, June

1955. 4 figs. , 4 refs. DLC--The principles of ionospheric

absorption apparatus, first designed by Sir E. APPLETON in

1935, are described with wiring diagrams. It employs a very

stable linear r-f pulse. (Met. Abst. 11E-118. )--C. E. P. B.

D-632 Piggott, W. R. (Radio Res. Station, Slough), Absorption

measurements during an eclipse. (In: Solar eclipses and the

ionosphere: a symposium. . . ed. by W. J. G. Beynon and G. M.

Brown. London, Pergamon, 1956. p. 106-115. 6 figs.

,

table, 12 refs. , 7 eqs. ) DWB--The measurement and interpretation of the changes in intensity of radio waves reflected

from the ionosphere during an eclipse present many difficulties. Some methods of overcoming these are discussed and

applied to observations made at Ibadan, Nigeria, during the

eclipse of Feb'. 25, 1952. It is found that the eclipse perturbation of the absorbing region implies a distribution of

ionizing radiation over the sun's disk closely similar to

those found for the E and Fl layers during the same eclipse.

(Met. Abst. 9. 6-265. )--Author's abstract.

D-633 Pisareva, V. V. (Gor'kii St. Univ. ), Fluctuations in the intensity of radio emissions scattered by coronal irregularities . Soviet Astronomy AJ, N. Y. , 3(3):419-424, Dec. 1959. fig.,

12 refs. , 10 eqs. DLC. Transl. of O kolebaniiakh intensivnosti radioizlucheniia, rasseiannogo na koronal'nykh neodnorodnostiiakh, Astronomicheskii Zhumal, Moscow, 36(3):

427-433, May/June 1959. DLC--

231
Simultaneous observations of solar radio emissions made at

two points separated in longitude (Gor'kii and Irkutsk) at a frequency of 260 Mc, are described. The experiment was

carried out in order to detect fluctuations in intensity of diffractive origin. The observations failed to reveal any fluctua

tions at a precision of up to 2% of the mean level of solar ra- dio emissions. The circumstance may be associated with the

fact that radio emission sources on the sun are of too large

angular dimensions. It is shown that observations made with

an antenna having an effective area of the order of 200 m^,

and an equipment with a fluctuation threshold of 2 sensitivity, with a time constant of 1 sec, might have led to the detection of such fluctuations even for wide angle sources. The

variation in the distribution is considered for an angle of ra- diation passing through a layer containing irregularities, as

a function of the distance of the observer to the layer. The

results obtained are applied to the scattering of radio emission from Tauri A on coronal irregularities. It is shown that

at great distances from the center of' the sun, the apparent

increase in the size of the source is not to be explained by

scattering on coronal rays. It must be assumed that there

also exist irregularities of finer scale in the corona. (Met.

Abst. 11L -88.) --Author's abstract.

D-634 Poeverlein, H. , Peculiar wave propagation characteristics

of a plasma with constant magnetic field. Planetary and

Space Science, N. Y. , 6:222-223, June 1961. Abstract only.

The paper was presented at the Plasma Sheath Symposium,

Boston, Mass. , Dec. 7-9, 1959. --A wave propagation theory

based on a study of the conductivity of a plasma shows that

with a sufficiently strong constant magnetic field the refractive indices arc in the order of one and independent of the

electron concentration. The conductivity of a plasma with

constant magnetic field is an asymmetric tensor. There is

no system of three principal directions for which the current

density components would be proportional to the electric

field strength components. This simple proportionality is,

however, found in a coordinate system whose coordinates are a vector in the direction of the magnetic field and two vectors rotating in either sense around the magnetic field direction. The longitudinal conductivity, that is, the conductivity in the magnetic field direction, is predominant. The

transverse conductivities now will be assumed being suppressed by the magnetic field. The propagation characteristics

then become independent of the electron concentration. The

two magnetoionic modes in this case have refractive indices

of or near 1, their attenuation is negligible, and one of them

is perfectly guided along the magnetic field lines. This peculiar type of propagation requires a magnetic field of sufficient

intensity, but no influence of ion motions or pressure gradients in the plasma.

232
D-635 Poincelot, Paul, Reflexion d'une onde electromagnetigue

plane sur un milieu ionise . (Reflection of a plane electromagnetic wave from an ionized medium. ) Academie des

Sciences, Paris, Comptes Rendus, 241(2): 186-188, July 11,

1955. 2 refs. , 15 eqs. Also his: Reflexion d'une onde

electromagnetigue plane sur un gaz ionise suivant une cer- taine loi. (Reflection of a plane electromagnetic wave from

an ionized gas according to a given law. ) Ibid. , 241(3):

290-292, July 18, 1955. 14 eqs. Also his: Reflexion d'une

onde electromagnetigue plane sur un gas ionise. (Reflection

of a plane electromagnetic wave from an ionized gas. ) Ibid.

,

241(9): 649-651, Aug. 29, 1955. ref. , eqs. DLC -Reflection

of plane electromagnetic waves is treated mathematically,

considering pulse frequency and structure of the reflecting

ionized medium (electronic density, height, etc.). The

analysis involves Hankel functions and their asymptotic developments. (Met. Abst. 8. 8-195. )-.-G. T.

D-636 Pope, Joseph H. , An investigation of whistlers and chorus

at high latitudes. Alaska. Univ. Geophysical Institute,

Contract AF 19(604) -1859, Scientific Report, No. 4, April

1959. 38 p. 18 figs. , table, 10 refs. -The whistlers and

chorus received at College, Alaska, during the period from

Dec. 1955 through March 1958, are studied particularly with

respect to temporal variations. The diurnal curves for whistler activity show maxima after midnight local time while the

seasonal variation peaks during the winter. It appears that

these variations in whistler activity are in part explainable

in terms of very low frequency propagation conditions. The

diurnal variation of chorus shows a maximum at about 1400

hrs local time. By the use of data from lower latitude stations a dependence of this time of diurnal maximum on the

geomagnetic latitude of the station is shown. The coefficients of correlation for chorus activity versus magnetic activity were determined on a monthly basis. A seasonal variation in these correlations is indicated which appears to be

unique for the geomagnetic latitude of College. A preliminary statistical study of one of the more easily measured characteristics of chorus is discussed. The characteristic chosen

is the mid-frequency in an element of chorus. A diurnal variation in this parameter is indicated. (Met. Abst. 11. 12-330.)

--Author's abstract.

D-637 Pope, J. H. (Geophys. Inst. College, Alaska), Effect of

latitude on the diurnal maximum of 'dawn chorus'. Nature,

London, 185(4706) :87-88, Jan. 9, 1960. 2 figs. , table, 6

refs. DWB--ALLCOCK and POPE have shown diurnal maxima

as a function of geomagnetic latitude. The observations from

a large number of stations with a time resolution of 1 hr during IGY makes it desirable to reconsider the latitude effect.

233
Our results indicate that it is desirable to consider the use

of the eccentric dipole field in connection with theories of

chorus. Also, the paths of whistler propagation may be affected by the eccentric field rather than the centered field,

which may be an important consideration from the point of

view of conjugate point experiments and electron density

computations. (Met. Abst. 11. 12-331. )--E. Z. S.

D-638 Pope, J. H. and Campbell, W. H. (both, Univ. Alaska),

Observations of unique VLF emission. Journal of Geophysical Research, Wash., D. C, 65(8): 2543-2544, Aug. 1960.

3 figs. , 3 refs. DLC- -Describes an unusual natural electromagnetic disturbance in the VLF range received at a low

noise site (64°43'N, 148°30'W) near College, Alaska. Sonagrams are shown. As the sound reminded the observers of

ocean breakers the name surf is suggested. Surf phenomenon is difficult to understand in terms of the present state of

knowledge and cannot be explained by the whistler echo

type of propagation. Surface exhibits systematic behavior

and is distinctive. (Met. Abst. 11. 12-333. )--E. Z. S.

D-639 Porter, Richard W. (General Electric), Rocket and satellite programs. American Museum of Natural History, N. Y.

Hayden Planetarium, Contributions, Ser. 1, No. 1:10-17,

1958. DWB (551 A512co) -Details of the U.S. rocket and

satellite plans for IGY which include study of atmospheric

pressure, temperature, density and winds, aurora and airglow, ionosphere, meteorology, geodesy, radio and the

launching and tracking stations, etc. , are discussed at

some length. (Met. Abst. 11. 2-81. )--M. R.

D-640 Powell, C.F. (Univ. of Bristol), Experiments on cosmic

radiation by means of artificial satellites . Royal Society

of London, Proceedings, Ser. A, 253(1275):482-487, Dec.

29, 1959. DWB, DLC --The paper presents some problems

of the cosmic ray radiation research to which an adequate

satellite program would make a valuable contribution. The

satellite could provide means for 1) the observation of nucleon-mucleon collisions in the region of extremely high energies, 2) investigation of the origin of cosmic rays, and

3) detection of X-ray radiation. (Met. Abst. 11. 12-205. ) --E. K.

D-641 Pravda, Moscow, Soviet artificial earth satellites: some

results of the scientific investigations carried out by the

two first Soviet sputniks. Transl. of original Russian in

Pravda, April 27, 1958. 12 p. Reproduction of typescript.

DWB (629. 1388 S729)-From the successful launching of

sputniks by the U. S. S. R. during 1957, scientists have been

better able to study the upper atmosphere and cosmic space.

234
Results of ionospheric and cosmic rays investigations have

been obtained from the data transmitted from these sputniks.

This paper discusses also the results of the medico-biological investigation of Sputnik II. The major part of the report

is the analysis of the results of these satellites. (Met.

Abst. 11. 2-35.) -N.N.

D-642 Prew, Henry E. , Space exploration: the new challenge to

the electronics industry. Journal of Astronautics, 4(1):9-11,

Spring 1957. 4 figs. , eqs. DLC--A lecture delivered at the

3rd annual meeting of the American Astronautical Society,

New York, N. Y. , Dec. 6-7, 1956. Concept of the research

vehicle is a rocket with a two way radio link, performance

and parameters of which are discussed. The radio system

should operate up to Mars (50 million miles). The radar

beacon data link, with earth based 500 Mc radars and 2 KW

output would suffice for moon orbit; 6 Megawatt for Mars

orbit. Earth transmitters would require 200 KW and 600

Megawatt power output, respectively. --W. N.

D-643 Priester, W. , Himmelskarte der 200 MHz-Strahlung. (Sky

chart of 200 MHz radiation.) Umschau, Frankfurt a.M.

56(16):485-487, Aug. 15, 1956. 4 figs. , 6 refs. DLC--

Radio radiation can penetrate the dust clouds which obscure

part of the Milky Way, and so give a complete picture. Isophotes are given on 200 MHz of the whole heavens, combining those obtained by F.DROGE and W. PRIESTER at Kiel and

by C. Wn ALLEN and C. S. GUM at Canberra. This gives radiation temperatures ranging from <120 to y- 1200 K. Most of

the cosmic radiation originates in our own Galaxy. The maximum is in a turbulent ionized gas cloud in colliding star systems in Cygnus A. (Met. Abst. 9A-129. )-C. E.P.B.

D-644 Priester, W. ; Bennewitz, Hans-Gerhard and Lengrusser,

Peter, Radiobeobachtungen des ersten kunstlichen Erdsatelliten . (Radio observations of the first artificial satellite.)

Arbeitsgemeinschaft fur Forschung des Landes NordrheinWestfalen, Wissenschaftliche Abhandlungen, Vol. 1, issued

Cologne (Westdeutscher Verlag), 1958. 38 p. 21 figs. , 4

tables, 5 refs. , 29 eqs. DLC (QC802. B64P7). Review by

S. F. Singer, Physics Today, 11(7), July 1958. --Trajectory

data and their time variations due to precession and to friction in the earth's atmosphere were calculated from measurements of Doppler effect and recordings of signal field strength

at 20 and 40 MHz. The trajectory data are presented. For

the precession of the trajectory, the authors obtained 2. 96 +

0. 20 /d in good agreement with the theoretical value of

D. G. KING-HELE and D. M. C. GILMORE. For atmospheric

limits at 215 km (over the mean globe (R = 6371 km) at 42°N

lat. ), a value of 4. 7. 10-13 g Cm"3 was obtained. This value

235
is five times as large as the density obtained for that altitude from American rocket experiments in 1952/53. (Met.

Abst. HJ-137.)--Transl. of authors' abstract (G. T.).

D-645 Priester, W. , Radiobeobachtungen des ersten kunstlichen

Erdsatelliten. (Radio observations of the first artificial satellite. ) Die Sterne, Leipzig, 34(3/4):64-69, 1958. 4 figs.

DLC--The 20, 005 and 40, 002 MHz signals of the first satellite have been observed and registered at many places; at

the laboratory of the Bonn University, the impulses of the

satellite were received on Oct. 5, 1957 at 05 h 22 U. T. and

registered on Oct. 6, 1957 (figure gives the registered

curves). The observations were developed to fix the satellite orbit and also to determine the variations of the orbits

elements. Observations made: 1) recording of the 20, 005

MHz field value; 2) recording of the 40, 002 MHz field

value; 3) measurement of Doppler effect. From the first

registrations and using Soviet information giving a declivity

of 65 for the orbit, a first approximation of the evolution of

the orbit is calculated. A figure gives a diagram for the determination of the height of the satellite and another figure

shows the decrease of air density with height. (Met. Abst.

11J-138.)--A.V.

D-646 Priester, W. , Sonnenaktivitat und Abbremsung der Erdsatelliten. (Solar activity and deceleration of earth satellites.

)

Die Naturwissenschaften, Berlin, 46(6): 197- 198, March 1959.

fig. , 6 refs. DLC--The object of the author is to stress the

remarkable correlation between the irregular fluctuation in

the rotation time of satellite 1957 Beta (Sputnik 2) and the

variation in radio radiation in the 20 cm band during Dec.

1957 and Jan. 1958. The article mentions a statement of

JACCHIA, BRIGGS and NONWEELER. (Met. Abst. 11. 12-

554.)-A.V.

D-647 Primich, R.I. (Def. Telecom. Estab. , Ottawa), Microwave

techniques for hypersonic ballistic ranges. Planetary and

Space Science, N.Y. , 6:186-195, June 1961. 17 figs. , 11

refs. , eqs. DWB--Describes two simple techniques and the

instrumentation developed and used to measure the properties of plasma generated by hypersonic projectiles. The Defence Research Telecommunication Establishment (DRTE) at

Ottawa, and the Canadian Armament Research and Development Establishment (CARDE) at Quebec City, are engaged

in a joint program of research into plasmas. --W. N.

236
D-648 Rabben, H. H. (Fraunhofer Inst. , Freiburg i. Br. ), Solare

Bursts der Type HI und ihre Beziehungen zu den Eruptionen. (Solar bursts Type III and their relation to eruptions. ) Zeitschrift Mr Astrophysik, Berlin, 49(2):95-110, 1960. 5 figs.,

6 tables, 14 refs. , several eqs. English summary p. 95.

DLC--136 burst events of Type III have been recorded with

the Freiburg radio spectrograph in a period of 200 hrs. Their

relation to 372 flares observed in the same period is studied.

By the use of records obtained at other observatories, the

spectral range was extended down to microwaves. About

20% of the flares coincided with Type III bursts, 88 of the

remaining 96 burst events occurred within the lifetime of

flares extended by + 5 min. It was found that: a) the greater the flare importance the greater the number of bursts per

event, b) Great burst events obviously occur near the onset

of a flare, while the occurrence of smaller events is independent of the flare's phase, c) Burst intensity and frequency drift/sec increase with the total spectral range of the

burst, d) The center limb decrease of the number of bursts

exceeds that of flares and in addition shows a strong eastwest asymmetry, e) The contribution of bursts of medium

intensity and frequency drift/sec increases strongly with

central meridian distance, f) The radio efficiency of flares

increases with importance, g) Burst producing flares prefer

certain centers of activity. (Met. Abst. 11L -100.) —Author's

abstract.

D-649 Radhakrishnan, V. and Roberts, J. A. (both. Radio Obs.

,

Calif. Inst, of Technology), Polarization and angular extent

of the 960 Mc/sec radiation from Jupiter. Physical Review

Letters, N.Y. , 4(10):493-494, May 15, 1960. table, 7 refs.

DLC--If the emission of intense 10 cm radiation from Jupiter

has its origin in a "Van Allen belt" surrounding Jupiter, the

angular extent of the source of the radiation is likely to be

several times the diameter of the planet. Some degree of

polarization of the radiation would be expected. These predictions are being tested with a variable spacing interferometer, and some results are reported. The source is strongly

linearly polarized, the radiation with the electric vector parallel to the equatorial plane of the planet being approximately 1. 7 times as intense as in the orthogonal polarization.

The radiation comes from a region several times the diameter

of the disk and is more strongly polarized in the outer parts.

(Met. Abst. 11. 12-66. )--E. Z.S.

237
D-650 Radhakrishnan, V. (Calif. Inst, of Tech. Radio Obs. , Owens

Valley), Self-absorption in the 21 cm radiation from galactic

neutral hydrogen. Astronomical Society of the Pacific, San

Francisco, Publications, 72(427):296-302, Aug. 1960. 3 figs.,

7 refs. , 2 eqs. DLC--The existence of clouds of neutral hydrogen at temperatures of galactic H 1 regions causes the occurrence of self absorption in the 21 cm radiation. This is substantiated by the observation reported in this paper in which

self absorption due to hydrogen was detected at a temperature

no greater than 60 K. The observations were made on two

nights with a frequency switched radiometer in conjunction

with a 90 ft equatorially mounted paraboloid. Samples of different types of 21 cm records related to these observations are discussed and graphically illustrated. (Met. Abst. 11L-114. ) -I. S.

D-651 Radio Astronomy Symposium, Jodrell Bank, Aug. 1955, ( Abstracts in English of a selection of papers, delivered at this

Symposium. ) Each abstract repaged. figs. , tables, refs.

,

eqs. Photostats of typescript. DWB (621. 384 I61p) -This

collection of photostats prepared from working papers of the

Jodrell Bank symposium on radio astronomy contains eleven

papers submitted by the Russian delegation (also one from

Czechoslovakia and one from Japan). All abstracts are in

English; they are either complete texts or extensive summaries

including numerous data and mathematical deductions. The

subjects discussed are methods used by Soviet scientists for

identifying and analyzing solar, planetary and galactic radio

radiation and results achieved in interpreting the mechanisms

producing such radiation. As a whole, the collection conveys

a good idea of the present state of Soviet research in the field

of radio astronomy. The length of the papers (or summaries)

varies between 2 and 12 typewritten pages. The titles are as

follows: Abstract No. 3, Link, F. : Possible proofs of the

lunar atmosphere. No. 32, Getmantsev, G. G. ; Stankevich,

K. S. and Troitskii, V. S. ; Detection of monochromatic radio- emission of deuterium from the center of the Galaxy on wavelengths of 91. 6 cm. No. 33, Ginzburg, V. L. : The nature of

cosmic radio emission and the origin of cosmic rays. No. 34,

Troitskii, V. S. and Khaikin, S.E. : Radio emission from the

moon and the nature of its surface. No. 35, Shklovskii, I. S. : Optical emission from the Crab nebula in the continuous spectrum. No. 36, Shklovskii, I. S. : Some problems of the meta- galactic radio emission. No. 37, Vitkevich, V. V. : Results

of observations of the scattering of radio waves on the elec - tronic inhomoqeneities of the solar corona. No. 38, Vitkevich,

V.V. : Disturbed radio emission from the sun as a sum of small

monochromatic peaks. No. 52, Hatanaka, Takeo: Polarization

of solar radio bursts. No. 61, Chikachev, B. M. : A survey of

Soviet observations of the radio emission from the sun during

238
solar eclipses . No. 62, Shain, C. A. ; Pickelner, S. B. and

Ikhsanov, R. N. : The measurement of the polarization of the

Crab nebula. No. 63, Vitkevich, V. V. : Burst of solar radio

emission on Sept. 26, 1952 . No. 64, Shklovskii, I. S. : On

the nature of the emission from the galaxy NGC 4486. (Met.

Abst. 11. l-66.)--G.T.

D-652 Ramanathan, K. R. ; Bhonsle, R. V. ; Kotadia, K. M. and

Rastogi, R. G. , The great solar flare of Feb. 23. 1956 and

associated ionospheric effects at Ahmedabad. Indian Academy

of Science, Proceedings, Sec. A, 43(5):306-308, May 1956. -

25 Mc/s cosmic noise fadeout and ionospheric soundings at

the time of a great solar flare. --CSIRO Abstract.

D-653 Ramanathan, K. R. and Bhonsle, R.V. (both, Physical Res.

Lab. , Ahmedabad, India), Cosmic radio noise absorption on

25 Mc/s and F scatter. Journal of Geophysical Research,

Wash. ,D.C, 64(10): 1635- 1637, Oct. 1959. fig, 4 refs. DLC

--An evaluation of the mean diurnal and seasonal variations of

the attenuation of cosmic radio noise in the atmosphere is attempted. The features examined are: minimum attenuation oc- curs before sunrise; daytime maximum near afternoon; a second maximum usually between 20 and 22 hrs, "in the winter

equinoctial and months.*' D region absorption and F region absorption in the ionosphere were separately estimated. D re- gion absorption depends directly on solar zenith distance. The

deviate F region attenuation was evidently connected with F

scatter. This view is strongly supported by observations of

BATEMAN and others in the Philippines-Okinawa area during

IGY. The frequency of evening enhancements reached a peak

during each equinoctial period, operating at 36. 4 Mc/s. The

peak at autumn could be observed during operations at 49. 84

Mc/s only. BATEMAN and his co-authors suggested that the

enhanced signal was propagated via the F region, and was en- hanced when there was low latitude spread F. The authors of

the present paper believe that ion clouds in the F region can

increase the scattered VHF signal strength from a ground transmitter, and attenuate at the same time the noise signals from

extraterrestrial noise sources. The decrease of cosmic noise

absorption on 25 Mc/s at Ahmedabad, on days with magnetic

storms, correlates with the absence of F scatter on magnetically disturbed days in low latitudes. The diagrams show the

monthly mean hourly values of total attenuation; D absorption

and an F2 attenuation of cosmic radio noise on 25 Mc/s at

Ahmedabad. (Met. Abst. 11. 12-68. )«O.T.

239
D-354 Ramanathan, K. R. ; Bhonsle, R.V. and Degaonkar, S. S,

(all, Physical Res. Lab. , Ahmedabad, India), Effect of electron-ion collisions in the F region of the ionosphere on the absorption of cosmic radio noise at 25 Mc/s at Ahmedabad:

changes in absorption associated with magnetic storms . Journal

of Geophysical Research, Wash., D. C. , 66(9): 2763-2771, Sept.

1961. 6 figs. , table, 18 refs. , 4 eqs. DLC—Measurements of

cosmic radio noise at 25 Mc/s, being made at the Physical Research Lab. , Ahmedabad, since March 1957, have shown much

larger values of absorption than those observed by SHAIN and

MITRA in Australia. Thic fact, together with the empirically

known dependence of the absorption on the critical frequency

of the F region, and the effect of magnetic storms on the absorption found from the Ahmedabad observations have led us to ex- amine the different possible parameters that may affect cosmic

noise absorption. It is found that electron-ion collisions in the

F region, both below and above the level of maximum electron

density, contribute in a substantial way to the absorption of

cosmic radio noise. The values of hourly absorption due to collisions of electrons with neutral particles and with ions have

been calculated for a period of 6 days in Aug. -Sept. 1957,when

there were three magnetic storms. The results obtained show a depletion of electrons above F maximum on the day following

the commencement of the magnetic storm and a refilling on

later days. The results are discussed in relation to findings

from satellite observations about particle fluxes in the Van

Allen belts during magnetic storms. (Met. Abst. 13A-136. )--

Authors' abstract.

D-655 Rand, S. (Convair, San Diego, Calif.), Wake of a satellite

traversing the ionosphere . Physics of Fluids, N. Y. , 3(2): 265-

273, March/April 1960. 6 figs. , 2 refs. , 65 eqs. DWB--The

particle treatment is applied to a study of the structure of the

wake behind a charged body moving supersonically through a low density plasma. For the case of a body whose dimensions

are considerably smaller than a Debye length, a solution is obtained which is very similar in structure to the solution obtained by using the linearized fluid dynamics equation. For the

case of a disk whose radial dimensions are much larger than a Debye length, two conical regions are found in the wake. At

the surface of each of these cones, over thicknesses of the

order of a Debye length, the ion and electron densities are increased over their ambient values. Formulae for the electrohydrodynamic drag on a wire, and on a large disk are obtained.

(Met. Abst. 11. 12-535. ) -Author's abstract.

240
D-656 Rand, S. (Convair, San Diego, Calif. ), Damping of the satellite wake in the ionosphere. Physics of Fluids, N. Y. , 3(4):

588-599, July/Aug. 1960. 3 figs. , table, 10 refs. , 79 eqs.

DW6--Landau damping of the ion plasma oscillations which

constitute the wake of a line charge moving supersonic ally

through a low density plasma is studied. Maxwellian distribution functions in the ambient plasma for both electrons and

ions have been assumed. It is found that the damping is critical to the question of whether the electrohydrodynamic wake

produced by a satellite in the ionosphere is observable, unless

the electron temperature is at least an order of magnitude greater than the ion temperature. (Met. -Abst. 11. 12-536. )—Author's abstract.

D-657 Rao, B. Ramachandra and Murty, D. Satyanarayana (both. Ionospheric Res. Lab., Andhra Univ. , Visakhapatnam), A new

continuous wave radio method for the study of ionospheric

drifts. Journal of Scientific and Industrial Research, Sec. A,

New Delhi, 17(12), Special Supplement,' Dec. 1958. p. 63-67.

2 figs. , 2 tables, 3 refs. DWB, DLC--A simplified method is

described, involving transmission from a distant sender received by three simple vertical aerials at the corners of a right

angled triangle, signal strength being recorded side by side on

a photographic paper. Sectional view is given. Comparison

with other methods show that this method yields consistently

reliable results. Another advantage is that choice of proper

frequencies enables drift measurements at different ionospheric

locations from the very same receiving center. (Met. Abst.

11F-108.)»W.N.

D-658 Rao, B. R. and Ramana, K. V. V. (both, Ionospheric Res. Labc

Andhra Univ. , Visakhapatnam), Diurnal variation of ionospheric absorption on 5. 65 Mc/s at Waltair during the IGY.

Journal of Scientific and Industrial Research, Sec. A, New

Delhi, 17(12), Special Supplement, Dec. 1958. p. 56-58.

table, 9 refs. , 6 eqs. DWB, DLC—The equations used to obtain the ionospheric absorption by calculating comparatively

the amplitude of the echo received with the amplitude if the

ionosphere were a perfect reflector are given. Procedure and

equipment used during the period March-Aug. 1958, are described. Tabulated n values (cos x-index) vary from 0. 88 to

1. 75, average 1. 25 as against the theoretical 1. 5. (Met.

Abst. 11E-125.)-W. N.

D-659 Rao, B. R. and Bhagiratha Rao, E. (both. Ionospheric Res.

Lab. Andhra Univ. , Visakhapatnam), Effect of enhanced solar

activity on the F2 region drifts at Waltair. Journal of Scientific

and Industrial Research, New Delhi, Sec. A, 17(12), Special

Supplement, Dec. 1958. p. 59-62. fig. , table, 7 refs. DWB,

DLC241
This is the first systematic investigation of a problem of this

nature. The spaced receiver method used was modified by

using a triple beam oscillograph for recording the fading patterns, frequency 6. Mc/s. SWI as obtained June 1957 -June

1958 represented by 21 days are analyzed, first plotted separately, then mean curves were drawn. Daily variation of NS

and EW curves shows the NS variation to be considerably affected on SWI days when prominent solar flares were reported,

otherwise not. (Met. Abst. 11F-106. )--W. N.

D-660 Rastogi, R. G. ; Sheriff, R.M. and Nanda, N. G. (all, Physical Res. Lab. , Ahmedabad), Some measurements of the signal

strengths of radio waves reflected from the ionosphere during

the solar eclipses of June 30. 1954 and June 20, 1955. (In:

Solar eclipses and the ionosphere: a symposium. . . ed. by

W. J. G. Beynon and G. M. Brown. London, Pergamon, 1956.

p. 137-142. 7 figs. , ref. ) DWB--The signal strengths of radio

waves from B. B. C. transmissions on 15-07 Mc/s were measured

at Ahmedabad during the 1954 eclipse, with control observations on a few preceding and succeeding days. The signals,

which could have been either by two-hop or three-hop reflections, showed well marked increases in intensity during the

eclipse. The increase of signal strength is considered to be

due to a decrease of attenuation in the Fl layer. Similar measurements were carried out for the 1955 eclipse at Trivandrum,

on the radio transmission from Colombo on 4. 87 Mc/s directed

skyward, and at Ahmedabad 7. 19 Mc/s, Here again the signals showed well marked increases of strength during the

eclipse. In both cases the signal intensity returned to its

normal value well before the end of the eclipse. The reflections observed at Trivandrum could have been from Fl, if there

was an Fl layer. Near the geomagnetic equator, however, Fl

is not usually observable at this hour of the day. Probably

the reflection took place from F2, with decrease of attenuation

mainly in Fl. The reflections observed at Ahmadabad should

have been from E, and the decrease of attenuation during the

eclipse should have taken place below E. (Met. Abst. 9. 4-

257. )--Authors' abstract.

D-661 Rastogi, R. G. and Sethuraman (both. Physical Res. Lab.

,

Ahmedabad), Field strength measurements of radio waves during the partial solar eclipse of Dec. 14. 1955 at Ahmedabad.

Journal of Scientific and Industrial Research, Sec. A, New

Delhi, 15(7):303-305, July 1956. 2 figs. , 3 tables, 2 refs.

DWB, DLC--The results of field strength measurements made

at Ahmedabad during the partial solar eclipse of Dec. 14, 1955,

on radio transmissions from Bombay on 7. 24 and 9. 55 Mc/s

are described. The 7. 24 Mc/s waves are reflected from the E

layer, while the 9. 55 Mc/s waves penetrate E and are reflected from the F2 layer on normal days. During the eclipse, the

242
field strength of the 7. 24 Mc/s transmission decreased below

the value for normal days, while the 9. 55 Mc/s waves showed

increased field strength. The changes are explained in terms

of the vertical incidence frequencies of the waves and the critical frequencies of the ionospheric layers at Ahmedabad.

(Met. Abst. 8.9-328.) -Authors' abstract.

D-662 Rastogi, R. G. (Nat. Res. Coun. Postdoctorate Fellow), Magnetic control on the variations of the critical frequency of the

F2 layer of the ionosphere. Canadian Journal of Physics, Ottawa, 37(7):874-879, July 1959. 3 figs. , 16 refs. DWB, DLC

--The paper discusses the comparative influence of the true

magnetic and smooth geomagnetic latitudes on the diurnal and

latitudinal variations of the critical frequency of the F2 layer

(foF2) at low latitudes. The diurnal variations of foF2 are shown to differ considerably at stations having the same geomagnetic latitude, but the discrepancies disappear when the

true magnetic latitude is taken into consideration. The latitudinal variation of noon values of foF2 is also shown to present

discrepancies for low latitude stations in the geomagnetic latitudes plot, but on true magnetic latitude plots the points fall

regularly along a smooth curve. (Met. Abst. 11F-114. )--

Author's abstract.

D-663 Ratcliffe, J. A. , Radio astroromy. Nature, London, 169

(4296): 348-350, March 1, 1952. 2 figs. DWB--A general ac- count of radiation of radio frequencies from the stars and the

sun. The solar intensity corresponds to a temperature in cor- ona of about 1, 000, 000 K. (Met. Abst. 4. 9-110. )-C.E. P.B.

D-664 Ratcliffe, J. A. , Microscopic mechanism for the absorption of

radio waves in the ionosphere. (In: Beer, Arthur (ed. ), Vistas

in astronomy, pub. London, 1955-1956. Vol. 2:791-798. 5

figs. , 2 refs. , 30 eqs.) DWB, DLC--The paper deals with the

absorption which occurs when a radio wave passes through a medium containing free electrons which make collisions with

heavy particles. It is shown that the absorption can be ac- counted for in terms of the impulses which the electrons ra- diate at each collision under the influence of the imposed

wave. Although these impulses are randomly timed they cor- respond to a coherent wave of the required amplitude and

phase. (Met. Abst. 11E-128. )- -Author's abstract.

D-665 Ratcliffe, J. A. (Cavendish Lab. , Cambridge Univ. ), Information by radio from the satellites. Institution of Electrical Engineers, London, Journal, 4(47): 603-608, Nov. 1958. 7 figs.

,

table, 2 refs. DLC--This article is a condensed form of a lecture dealing with some exploratory results of ionospheric re- search as obtained by way of radio signals from orbiting satellites, especially Sputnik I. The propagation characteristics

243
of the 20 and 40 Mc/s radio waves used permit deductions to

be drawn with regard to orbital features, ionospheric electron

content, density and distribution, influence of earth's magnetic field, etc. Results deduced from the Doppler effect and

the Faraday effect are discussed and shown in graphs. (Met.

Abst. 11E-127.)--W. N.

D-666 Ratcliffe, J. A. et al. , Transition from the ionosphere to in- terplanetary space. Geophysical discussion of the Royal

Astronomical Society, Feb. 21, 1958. Geophysical Journal,

London, l(3):263-266, Sept. 1958. DWB, DLC-Under chairmanship of J. A. RATCLIFFE, a discussion was held at the

Royal Astronomical Society headquarters. SYDNEY CHAPMAN

spoke on his static theory of heating of the outer atmosphere

by the solar corona. D. E. BLACKWELL discussed optical observations of the zodiacal light. J.V.EVANS, of Jodrell Bank

Observatory, spoke on radio echoes from the moon. K. WEEKES,

of Cavendish Laboratory/ Cambridge University, reported on

ionospheric deduction based on satellite observations and J. A. RATCLIFFE summarized work on whistlers and radio frequency atmospherics at Stanford and Boulder, Colo. A.HEWISH

discussed observations of radio stars (made at Cambridge) observed through the solar corona. (Met. Abst. 11.7-41.)--

M.R.

D-667 Ratcliffe, J. A. (Univ. of Cambridge), The magneto-ionic

theory and its applications to the ionosphere. London, Cambridge Univ. Press, 1959. 206 p. figs. , tables, eqs. , bibliog. p. 193-201. Price 40 sh. DLC (QC661. R33). Review

in Royal Meteorological Society, Quarterly Journal, 85(365):

320, July 1959. Review by A. Scibor-Rylski in Science Progress, London, 47(188): 776-777, Oct. 1959. Review by G.H.

Munro in Australian Journal of Science, Sydney, 22(4): 176,

Oct. 1959. --Account of the theories of radio wave propagation

through the earth's ionosphere and through the ionized envelopes of radio stars, being concerned with the propagation of

electromagnetic waves through a partially ionized gas in the

presence of a magnetic field. The author is not content to

follow a simple mathematical approach but searches for physical reasons for the behavior of the xvaves. Two approaches

have been adopted: a macroscopic one in which the properties

of the medium are averaged out and a microscopic one based

on the motion of individual electrons. Ch. I treats the derivation of the equations, the microscopic approach, the physical

reason for the characteristic waves and their dispersion, the

absorption on the "Macroscopic" theory and the microscopic

picture of absorption. In Pt. II, the results are summarized

in graphical form and simple rules demonstrated for computing

curves of refractive index and absorption index as functions

of electron density. Pt. Ill treats application of the theory to

244
the earth's ionosphere and mentions a wide range of phenomena capable of explanation in terms of the magneto-ionic

theory of a homogeneous medium. Finally, the author discusses a number of relevant miscellaneous topics, including

the relationship between the anisotropic behavior of the atmosphere and that of transparent crystals. A complete bibliography and an alphabetical index of subjects are included

in this excellent work. (Met. Abst. 11. 1-17. )«A. V.

D-S68 Ratcliffe, J. A. (ed. ), Physics of the upper atmosphere. N. Y..

Academic Press, 1960. 586 p. figs. , tables, refs. , eqs.

Review by M. G. Morgan in Institute of Radio Engineers, N. Y.

,

Proceedings, 48(12):2045, Dec. 1960. Review by E. V. Apple- ton in Journal of Atmospheric and Terrestrial Physics, London,

19(3/4):295, Dec. 1960. Contents: Chapman, Sydney, The

earth's outermost atmosphere, p. 1-16. Nicolet, Marcel, The

properties and constitution of the upper atmosphere, p. 17-71.

Newell, Homer E. , Jr. , The upper atmosphere studied by rockets and satellites, p, 73-132. Friedman, Herbert, The sun's

ionizing radiations, p. 133-218. Bates, D. R. , The airglow.

p. 219-267. Bates,' D. R. , General character of auroras.

p. 269-296. Bates, D. R. , The auroral spectrum and its interpretation, p. 297-253. Booker, Henry G. , • Radar studies

of the aurora, p. 355-375. Ratcliffe, J. A. and Weekes, K.

,

The ionosphere, p. 377-470. Vestine, E. H. , The upper atmosphere and geomagnetism, p. 471-512. Greenhow, J. S. and

Lovell, A. C.B. , The upper atmosphere and meteors, p. 513-

549. Chapman, Sydney, Newell, Homer E. , Jr. et al. Advances during the International Geophysical Year, 1957/1958^

by authors of various of preceding articles, p. 551-563. DWB

(M10. 5 R233ph)--This excellently edited collection of articles,

reviewing current knowledge of the atmosphere above 60 km,

consists of the 12 above cited chapters written by well-known

authorities on the physics and chemistry of the upper atmosphere. It includes knowledge of the aurora, airglow, ionosphere, meteors, and geomagnetism gained from direct and indirect methods — rockets and satellites, etc. , mainly before

IGY but with supplementary information obtained during 1857/

1958 and even 1959. Recent advances in knowledge of the

Van Allen Belts, radar studies of the aurora and solar ionizing

radiations are treated in the final chapter written by various

authors on the results of IGY. The articles as a whole contain a great deal of theoretical, as well as experimental, re- sults. An extensive author index, including references to

authors referred to in the bibliographies, and a subject index

are provided. (Met. Abst. 12. 4-1. )--M. R.

245
D-669 Rawer, Karl, Die Ionosphare: ihre Bedeutunq fur Geophysik

und Radioverkehr. (The ionosphere: its importance in geophysics and radio communication. ) Groningen, P. Noordhoff,

1953. 179 p. 67 figs. , 143 refs. , 68 eqs. DLC--A complete

text on the use of radio in ionospheric research. Ch. I takes

up methods of observation by echoes, spectroscopic methods

for aurora and airglow, magnetic, meteor and luminous night

clouds, and soundings; Ch. II gives results of observations

by echo methods, magnetic data, composition, pressure, density and temperature. Ch. Ill discusses theories of ionospheric stratification (origin and disappearance of ionization

and explanation of different layers. Ch. IV takes up normal

and irregular changes of the ionosphere (D, E, F2, F, E2, G and

Es and influence of magnetic storms, eclipses, polar summer

and night, commencements). Ch. V discusses influence of

ionosphere on propagation of radio waves and forecasting propagation. (Met. Abst. 11B-118. )--M.R.

D-670 Rawer, K. (Ionospheric Stat. , of S. P. I. M. , France), Some

remarks concerning ionospheric absorption work. Journal of

Geophysical Research, Wash., D. C. , 60(4): 534-535, Dec.

1955. fig. DLC --Monthly mean absorption decrements in E

layer, as well as daily values, do not support assumption of a horizontally stratified plane ionosphere whose total absorption is characterized by an effective reflection coefficient.

Focusing effects arising from curvature in the reflecting layer

produce an apparent reflection coefficient greater than 1. Effect is only important in vicinity of focusing areas. Night F2

observations showed negative absorption decrement in 30% of

cases. Even in daytime, 2 or 3 daily observations show important focusing. These areas are illustrated as being in the

form of inverted ripples. (Met. Abst. 11E-129. )—M. R.

D-671 Rawer, K. (Service de Prevision Ionospherique Militar, Frieburg). Absorption measurements for the eclipse of June 30,

1954. (In: Solar eclipses and the ionosphere: a symposium. . ed. by W. J. G. Beynon and G. M. Brown, London, Pergamon,

1956. p. 102-105. 6 figs. , 5 refs. ) DWB--Results are presented of field strength and virtual height measurements made

at Freiburg on frequencies of 2. 9 and 1. 95 Mc/s during the

partial eclipse of June 30, 1954. The different behaviors observed on the two frequencies are explained in terms of the

relative contributions of deviative and non-deviative absorptions. It is found possible to isolate these two types. Some

observations on 1. 95 Mc/s at oblique incidence are also described. (Met. Abst. 9. 6-266. )--Author's abstract.

246
D-672 Rawer, K. (Ionospharen Institut, Breisach/Rh. , Germany)

and Suchy, K. (Physikalisches Inst. d. Univ. Marburg/Lahn,

Germany), Whistlers excited by sound waves. Institute of

Radio Engineers, N. Y. , Proceedings, 49(5): 968-969, May

1961. fig. , 4 refs. DLC--This brief discussion is in favor of

Lippmann's view, since only strong waves, for example such

as from nuclear explosions, can produce observable transversal electromagnetic waves. This mechanism is summed up in

the conclusion drawn regarding excitation of whistlers by

sound waves in a plasma (here below 300 km). (Met. Abst.

unpub. )--W. N.

D-673 Reber, Grote, Cosmic static . Institute of Radio Engineers,

N. Y. , Proceedings, 28(2):68-70, Feb. 1940. 6 figs. , 14 refs.,

7 eqs. DLC--An attempt to account for the static from space,

particularly from the Milky Way, by means of brief quantitative calculations using Kramer's formula corrected for stimulated radiation. --W. N.

D-674 Reber, G. , Cosmic static . Astrophysical Journal, 100(3):

279-287, Nov. 1944. 5 figs. , 3 foot-refs. , 2 eqs. DLC--

Cosmic static is a disturbance in nature which manifests itself as electromagnetic energy in the radio spectrum arriving

from the sky. The results of a survey at a frequency of 160

Mc/s show the center of disturbance to be in the constellation Sagittarius. Minor maxima appear in Cygnus, Cassiopeiae, Canis Major, and Puppis. The lowest minimum is in

Perseus. Radiation of measurable intensity is found coming

from the sun. (Met. Abst. 9A-3. ) --Author's abstract.

D-675 Reber, G. , Motion in the solar atmosphere as deduced from

radio measurements. Science, 113(2934) :312-314, March 23,

1951. table, 10 refs. DLC--Disturbances in the variably ionized solar atmosphere generate radio waves of a transient nature, having different frequencies at different levels. These

radio frequencies are used to analyze the source of the motions within the solar atmosphere and their velocities during

a sudden ionospheric disturbance. (Met. Abst. 2.7-67.)--

I.L.D.

D-676 Reber, G. , Fine structure of solar radio transients. Nature,

London, 175(4446) : 132, Jan. 15, 1955. 6 refs. DWB-High

speed recordings on 480-51 Mc/s showed solar bursts to be

made up of numerous small transients (pips), the structure

and duration of which are described. There is a fundamental

relation between their mode of generation, source in the solar

atmosphere, and duration. (Met. Abst. 9A-90. )--C.E. P. B.

247
D-677 Reber, G. , Radio astronomy in Hawaii. Nature, London,

175(4445): 78-79, Jan. 8, 1955. DWB--Observations of cosmic

static at 10, 020 ft on summit of Haleakala, Maui, are described. Sources in Cassiopeia and Cygnus show interference patterns at 100 Mc/s and considerable asymmetry. (Met. Abst.

9A-91.)-C.E.P.B.

D-678 Reber, G. (Research Corp. , N. Y. C. ) and Ellis, G. R. (Commonwealth Obs. , Hobart, Tasmania, Australia), Cosmic ra- dio frequency radiation near one megacycle. Journal of Geophysical Research, Wash., D. C. , 61(1):1-10, March 1956.

9 figs. , 4 refs. DLC--Observations were made of cosmic ra- dio frequency radiation on frequencies of 2130 kc/sec, 1435

kc/sec, 900 kc/sec, and 520 kc/sec. Using fast photographic recording with a cathode-ray indicator, a method of recording was found which effectively reduced interference from atmospherics. The maximum intensity of the cosmic radiation

at 2130 kc/sec was approximately 10*19 watt per square meter

per cycle per sec (W. M. "^c/s'-) per steradian, with an estimated error of 50%. At the other frequencies, the results were

more uncertain, although the intensities were of the same ord- er of magnitude, with perhaps lower intensities at lower frequencies. The ionospheric effects associated with observations near the critical frequency are discussed. (Met. Abst.

9A-132. ) --Based on authors' abstract.

D-679 Reber, G. , Early radio astronomy. Institute of Radio Engineers, N. Y. , Proceedings, 46(l):15-23, Jan. 1958. 23 refs.

DLC--A history is given of radio astronomy experiments conducted by the author from 1936 through 1947. A description

of the parabolic reflector and equipment design along with

reasons for the choice of successive operating frequencies of

3300, 910, 160, and 480 Mc/s. The results are reviewed in

light of more recent knowledge. Published articles covering

the scientific details will be found in the (23) foot-notes.

(Met. Abst. unpub. ) --Author's abstract.

D-680 Reber, G. (National Radio Astronomy Obs. , Green Bank,

W. Va. ), Cosmic static at kilometer wavelengths. Canada.

Defence Research Telecommunications Establishment, Publication No. 1025, March 1960. p. 243-248. 4 figs. , ref.

DWB (M21 S989pro)--The theory of propagation of ionospheric

Y mode (extraordinary longitudinal) has been improved. Now

the theory is in better agreement with galactic observations

of cosmic static at 520 kc. The intensity per unit bandwidth

of cosmic static is still rising at 520 kc compared to 2130 kc.

Further experiments are discussed. (Met. Abst. unpub. )--

Author's abstract.

248
D-681 Reid, George C. and Leinbach, Harold (both. Geophysical

Inst. , Univ. of Alaska), Low energy cosmic ray events associated with solar flares. Journal of Geophysical Research,

Wash., D.C., 64(11): 1801-1805, Nov. 1959. table, 22 refs.

DLC--As a result of the IGY riometer program, it has been

found that the measurement of ionospheric absorption in arctic regions is a sensitive method of detecting low energy cosmic rays associated with solar flares. The normal morphology

of these events is described, and details are given of the 24

such events that have been detected in the period from May

1957 through June 1959. Two features have been noted: an

apparent asymmetry in the distribution of cosmic ray producing flares across the solar disk; a pronounced degree of uniformity in the distribution of the radio wave absorption over

the terrestrial polar cap. These features are discussed, and

tentative explanations are suggested. (Met. Abst. 11. 8-88.

)

--Authors' abstract.

D-682 Reid, G. C. and Collins, C. (both. Defence Res. Board,

Ottawa, Canada), Observations of abnormal VHF radio wave

absorption at medium high latitudes . Journal of Atmospheric

and Terrestrial Physics, London, 14(l/2):63-81, April 1959.

7 figs. , table, 23 refs. , eq. DLC--A study of cosmic noise

absorption at a frequency of 30 Mc/s at Ottawa and Churchill

has revealed the existence of two apparently distinct types of

abnormal absorption event. One of these is predominantly a

night time phenomenon and is closely associated with auroral

and geomagnetic disturbance. It is suggested that this absorption may be caused by an increase in electron collisional

frequency at £ region heights rather than by a large increase

in electron density at lower levels. The second type of absorption is confined to the auroral zone and is predominantly

a daytime phenomenon, recurring for several days after a

large solar flare. Evidence is presented to show that this

absorption is due to an increase in ionization at very low levels in the ionosphere. The cosmic noise measurements are supported by evidence from a number of VHF forward scatter

circuits in Canada, and this is used to obtain information

about the geographical extent and frequency of occurrence of

these abnormal absorption events. (Met. Abst. 11E-133. )--

Authors' abstract.

D-683 Reid, G. C. and Stiltner, E. , Design and use of a phasesweep interferometer for the study of radio star scintillations

in the auroral zone. Alaska, Univ. Geophysical Institute,

Contract AF 30(635) -2887, Supplement to Final Report (Phase

I), Feb. 1, 1960. 15 p. 13 figs. , 3 refs. , 5 eqs. DWB

(M94. 6 A323ra)--The usefulness of the phase sweep technique

in interferometers designed to record radio star signals is discussed. Interferometers of this type have been built for use

249
at frequencies of 223 and 456 Mcs, and their electronic design is explained in some detail. The report also includes a discussion of the automatic data processing system which

has been designed to operate in conjunction with the interferometers in the analysis of the amplitude scintillation of

radio stars. (Met. Abst. unpub. ) --Authors' abstract.

D-684 Reid, G. C. (Defence Res. Telecommunications Estab.

,

Shirley Bay, Ottawa, Canada), A study of the enhanced ionization produced by solar protons during a polar cap absorption

event. Journal of Geophysical Research, Wash. , D. C. , 66

(12):4071-4085, Dec. 1961. 17 figs. , table, 27 refs. , 22

eqs. DLC--Polar cap absorption of radio waves has been

shown to be caused by an influx of fast particles emitted by

the Sun at the time of certain solar flares. The steady-state

daytime and night-time electron density profiles produced in

the lower ionosphere by such a particle flux are calculated,

on the assumptions that the particles are protons and that „ their differential energy spectrum is of the form n(E) dE=KE"^ dE, with a sharp cutoff at the low energy end. The shapes of

the profiles are shown to be almost independent of the proton

spectrum and low energy cutoff, provided the latter is higher

than about 10 Mev. The radio wave absorption this ionization

would produce is calculated for frequencies of 30 Mc/s and

60 Mc/s. Conditions during the twilight transition period are also examined, assuming that O2" is the only negative ion present. The photodetachment coefficient of O2" is calculated as

a function of solar zenith angle, and corresponding electron

density profiles deduced. By comparing the absorption these

profiles would produce with the observed variation of cosmic

noise absorption during twilight, it is shown that the presence

of O2" alone is insufficient to account for the observations.

(Met. Abst. unpub. ) --Author's abstract.

D-685 Richey, Frances and Wehner, R.S. , Use of radar as an ion - ospheric probe. Plesset, E. H. ; Assoc, Inc., Los Angeles,

Contract AF 19(604) -6187, Scientific Report No. 1, Oct. 11,

1960. 25 p. 2 figs. , 14 refs. , eqs. DWB--The analytical

results discussed here show the feasibility of radar measurements of electron density and of collision frequency as a function of space and time, and under a variety of ionospheric disturbances. Cross modulation, discussed in some detail, is a technique applicable for extreme electron densities or collission frequencies; its expected usability at lower frequencies

is to be checked. --W. N.

250
D-686 Ringnes, Truls S. , Astronomiske begivenheter i 1953.

(Astronomical events in 1953.) Naturen, 78(14):418-429,

1954. 10 figs. DLC--The 11 progressive events which HARLOW SHAPLEY (Harvard Observatory) considers significant are summarized and discussed briefly: (1) establishment of the

National Astronomical Observatory in the U. S. ; (2) construction of the world's largest radio telescope at Jodrell Bank, Eng.

(3) electronic enlarger as developed by A.LALLEMAND and

M.DUCHESNE (France) and (4) the hypersensitive photometer

as developed by W. A.BAUM; (5) Radio astronomic research

into the Magellanic Cloud by F.J.KERR and J. V.HINDMAN

(Radio-physics Lab. , Sydney, Australia). This research

shows a turbulent movement around a joint center of gravity

at a relative speed of 45 km/sec. The cloud masses of the

large and the small clouds contain 10% and 3% water vapor,

respectively. The other subjects are: (6) revision of the extra galactic scale of distance; (7) asteroidal light curves;

(8) F corona and the zodiacal light; (9) relativistic gas dynamics; (10) Lyman-alpha line in the solar spectrum and (11) new

method for determining the electron density in the solar corona

as a function of dispersion of radio waves from irregular structure in the uppermost regions. (Met. Abst. 9B-100. )--W. N.

D-687 Rix, H. D. , Radio propagation and ionized gases: a survey.

Pennsylvania. State Univ. Ionosphere Research Lab. , Contract Da-36-061-ORD-577, Scientific Report, No. 123, Pt. A,

Sept. 1, 1959. 50 p. 2+3 figs. , 4 + 11+49 refs. , 22 eqs.

DWB (M10. 535 P415i)--This report surveys electromagnetic

wave propagation effects relating to the problem of radio interference encountered during powered flight of large missiles.

An expression for the absorption of a radio signal traversing

a plasma is developed from the approximate theory of plasma

conductivity. Results of more accurate treatments of conductivity theory are introduced by way of comparison. Equations

showing the effect of a magnetic field on the signal are also

given. Properties of several types of plasma—flames, gaseous discharges and shock waves—are described in terms of

methods of measuring electron density, mechanisms of ionization and means of controlling free electron concentration. Specific propagation effects treated include high frequency antenna breakdown and ionospheric effects. A guide to the relevant literature of these various subjects is provided. (Met.

Abst. 11. 12-482. )--Author's abstract.

D-688 Roberts, C.A. (Douglas Aircraft Co. ), Radio frequency radia - tion from hypersonic plasmas with impressed oscillating electric fields. Planetary and Space Science, N. Y. , 6:221-222,

June 1961. Abstract only. The paper was presented at the

Plasma Sheath Symposium, Boston, Mass. , Dec. 7-9, 1959. --

251
The total (integrated frequency distribution) radiated power

from a plasma with an impressed electric field (£ cos cot)

is calculated taking into account only the semi-classical

Bremsstrahlung due to electron ion encounters. The calculation is made by using the impulse approximation with the lower limit on the impact parameter taken as the de Broglie wavelength of the electron. The electron velocities are then aver- aged by using the appropriate non-equilibrium velocity distribution. Results are given for various conditions that might

be encountered in hypersonic plasmas. The radiation frequency spectrum of the plasma in the radio frequency range

for a zero field is then examined by a Fourier analysis of the

acceleration using the impulse approximation. In order to

determine the validity of the approximation, a comparison is

made between the zero field radiation spectrum from an ionized gas calculated by using the impulse approximation with

a cutoff at the de Broglie wavelength and the spectrum from

the exact (dipole approximation) calculation for low (radio)

frequencies. Possible effects on electronic and detection

equipment are briefly considered.

D-689 Roberts, C. R. ; Kirchner, P.H. and Bray, D. W. , Radio re- flections from satellite produced ionization. Institute of

Radio Engineers, N. Y. , Proceedings, 47(6): 1156-1157, June

1959. DLC—Using different frequencies, several disturbances

of signals from orbitting satellites were observed. Signal

characteristics and some speculations as to the causes are given. —W. N.

D-690 Roberts, J. A. (Div. of Radiophysics, C.S. I. R.O. Univ.

Grounds, Chippendale, N. S. W. ), Evidence of echoes in the

solar corona from a new type of radio burst. Australian Journal of Physics, Melbourne, ll(2):215-234, June 1958. 11 figs.,

2 plates, 11 refs. , eqs. DLC—A new spectral type of solar

radio burst is described. The bursts contain two elements,

the second being a repetition of the first after a delay of 1& - 2 sec. In each element the frequency increases with time at a

rate of 2-8 Mc/s per sec. The bursts are of very short duration and are confined to the longer meter wavelengths. Occasionally they occur within, and evidently form part of the

structure of a burst of spectral type III. It is suggested that

the second elements of the bursts are echoes of the first, re- flected from lower levels of the solar corona. If the burst

radiation is assumed to occur at the second harmonic of the

coronal plasma frequency, the delay between the elements

can be quantitatively explained providing the coronal density

gradient is 1-5 times steeper than in the Baumbach-Allen model.

Two alternative explanations of the rising frequency characteristic are considered. Either the exciting disturbances travel

252
4

in through the corona at speeds between 2 and 5 x 10 km

sec"^ , or the outward travelling disturbances responsible for

type III bursts encounter "hills" of electron density in the cor- ona. (Met. Abst. unpub.) --Author's abstract.

D-691 Roberts, J. A. and Stanley, G. F. (both, Calif. Inst, of Tech.

Radio Obs. , Owens Valley), Radio emission from Jupiter at a wavelength of 31 centimeters . Astronomical Society of the

Pacific, San Francisco, Publications, 71(423) :485-496, Dec.

1959. 4 figs. , 22 refs. , 3 eqs. DLC--This is a report of a series of observations at a wavelength of 31 cm and a discussion of their implications. The observations were made with

a 90 ft equatorially mounted radio telescope between April 15

and June 17, 1959. The observed intensities are graphically

represented. The paper does not arrive at any definite conclusion with respect to the origin of the high intensity decimeter radiation from Jupiter. (Met. Abst. 11L-104. )—I. S.

D-692 Roberts, J. A. (Div. of Radiophysics, C.S. I. R.O. , Univ.

Grounds, Chippendale, N. S. W. ), Solar radio bursts of spectral type II. Australian Journal of Physics, Melbourne, 12(4):

327-356, Dec. 19o». 16 figs. , 3 tables, 31 refs. DLC-The

characteristics of bursts of spectral type II are studied in a

sample of 65 bursts. Approximately half the bursts show harmonic structure and about half are compound type Ill-type II events. Band splitting, the doubling of both the fundamental

and second harmonic bands, is also relatively common. A

rather less common feature is the appearance of herring-bone

structure in which the slowly drifting band of the type II burst

appears to be a source from which rapidly drifting elements

diverge toward lower and higher frequencies. Statistics are given of the rate of occurrence of the bursts, their frequency

range, the rate of frequency drift, and the harmonic ratio.

Many of the type II bursts occurred near or after the maximum

of a chromospheric flare. However, only about 3% of flares

(of Class I or greater) are accompanied by type II bursts, although the figure rises to 30% for Class 3 flares. There is a

greater tendency for the geomagnetic field to be disturbed in

the few days following a type II burst than there is after large

flares which are not accompanied by type II bursts, or after

large radio bursts of spectral type III. Statistically the

greatest disturbance occurs after about two days, implying a mean speed of travel of about 1000 km/sec. (Met. Abst.

11. 12-57. ) --Author's abstract.

D-693 Roberts, Walter Orr (High Altitude Obs. , Boulder, Colo. ),

Solar-terrestrial relationships: weather and communications.

Smithsonian Contributions to Astrophysics, Wash. , D. C.

,

1(1):99-101, 1956. DLC--Several aspects of solar influence

are discussed and, in particular, the measured and the

253
probable influences upon world-wide weather patterns and

ionospheric radio communication. It is suggested that the

future practical stakes in short and long range weather forecasting may well surpass the expected gains within radio

communication forecasting. (Met. Abst. 9. 9-296. )--W. N.

D-694 Rochelle, R. W. , Signal-to-noise considerations for a space

telemetry system. Institute of Radio Engineers, N. Y. , Proceedings, 48(4):691-693, April 1960. 2 figs. (incl. photo),

2 refs. , 3 eqs. DLC--A signal-to-noise comparison is given

between the pulse frequency channels and the pulse width

channels for the FM/PDM-AM telemetry system. It is shown

that the pulse frequency channels have either a higher signalto-noise ratio or greater information rate capability than the

pulse width channels. (Met. Abst. 11. 12-488. )- -Author's

abstract.

D-695 Rosen, A.; Coleman, P. J. , Jr. and Sonett, C.P. (all. Space

Technology Lab. , Los Angeles, Calif. ), Ionizing radiation

detected by Pioneer II . Planetary and Space Science, N. Y. , l(4):343-346, Sept. 1959. 2 figs. , 3 refs. , eqs. DWB, DLC

--The total ionizing component of cosmic radiation was measured up to an altitude of 1550 km. An upper bound to the

ratio of average -to -minimum specific ionization was determined by comparing the ionization with the count rate observations from the Explorer IV satellite. This result implied that

protons are the predominant species which gave rise to the

observed ionization. (Met. Abst. 11. 12-206. ) --Authors'

abstract.

D-696 Ross, W. J. , Ionospheric investigation from satellite radio

observations Pt. 1, Doppler effect recording instrumentation.

Pennsylvania. State Univ. Ionosphere Research Lab. , Contract AF 19(604) -4563, Scientific Report No. 120, June 30,

1959. 81 p. 24 figs. , eqs. , 14 refs. DWB (M10. 535

P415i)--A brief survey is made of the main features of satellite transmitters and of the ionospheric propagation effects

produced in the radio waves from them. From these considerations, the desirable properties of the transmitter are summarized and the necessary properties of the receiving apparatus are inferred. Detailed descriptions of the various units

of the receiving instrumentation are then given, followed by

the presentation of a sample record analyzed to yield electron content of the ionosphere. (Met. Abst. 11F-117. )--

Author's abstract.

254
D-697 Ross, W. J. (Pennsylvania State Univ. ) f The determination

of ionospheric electron content from satellite Doppler measurements. Pt. 1. Method of analysis . Journal of Geophysical Research, Wash., D.C., 65(9): 2601 -2606, Sept. 1960.

5 refs. , 10 eqs. Pt. 2. Experimental results. Ibid. p. 2607-

2615. 9 figs. , 6 refs. DLC--A procedure for determining the

ionospheric electron content up to the height of an active satellite from Doppler data is developed. The equations derived

from first order theory are discussed and corrected separately

for earth curvature, large refraction, off zenith orbit, vertical

satellite motion, horizontal ionospheric variations, and the

effects of the earth's magnetic field. The methods were developed initially for use with the harmonic radiations from

satellite 1958 %z at frequencies of approximately 20 and 40

Mc/s, but may be adapted to other harmonic frequency ranges.

In Pt. 2, the preliminary results of the analysis of daytime

Doppler frequency records from satellite 1958 Sx for the period Sept. 1958 to Dec. 1959 are presented in the form of ionospheric electron content derived using the methods of part 1.

Strong seasonal effects are found, the content being lower

and the equivalent slab thickness greater in summer than in

winter. Magnetic control of the summer ionosphere content

is indicated, although the equivalent slab thickness is almost

constant. The values of content obtained agree fairly well

with the results of independent polarization rotation studies.

(Met. Abstract. 11. 12-375. )--Author's abstract.

D-698 Rosseland, Svein and Tandberg -Hanssen, Einar, On some

solar disturbances on Aug. 18 and Sept. 24. 1956. Astro

physica Norvegica, Oslo, 5(ll):279-287, March 1957. 9 figs,

(incl. photos), 2 tables, 3 refs. DWB--The correlation between solar radio bursts and high speed features on the sun

has been studied in some detail in two cases observed at

Harestua in 1956: (1) during the development of two dark

surges on Aug. 18 and (2) during the activation of the limb

prominence on Sept. 24. The motion of the prominence material has been analyzed relative to the position of the limiting isodiaphanous surface for the frequency in question, i. e. , 200 Mc/s. It is pointed out that the time correlation between

the occurrence of the radio bursts and the penetration of prominence material through the isodiaphanous surface is close

enough to support the view that the excess radio noise is generated in the moving prominence material. (Met. Abst. 10. 1-

243.) -Authors' abstract.

D-699 Rothwell, Pamela and McLlwain, Carl (both. State Univ. of

Iowa), Satellite observations of solar cosmic rays. Nature,

London, 184(4681): 138-140, July 18, 1959. 3 figs. , table,

11 refs. DWB--On Aug. 16-17, 23-24, 26-27, 1958, increases

in the intensity of charged particles outside the Van Allen

255
radiation zones were detected by Explorer IV satellite 1958

epsilon, at high magnetic latitudes and rather low satellite

altitudes (270-650 km). These increases are associated

with the large solar flares which are measured from balloons

and with riometers during the period. (Met. Abst. 11. 5-169. ) --N. N.

D-700 Rotman, W. and Meltz, G. (U. S. Air Force, Cambridge Research Laboratories), Experimental investigation of plasma

sheath properties of a re-entry vehicle. Planetary and Space

Science, N. Y. , 6:224, June 1961. Abstract only. The paper

was presented at the Plasma Sheath Symposium, Boston, Mass.,

Dec. 7-9, 1959. --The effects of the plasma sheath, which

surrounds a re-entry vehicle, upon the transmission and re- ception of radio signals will be investigated by means of an

instrumented nonablative nose cone to be flown in a re-entry

trajectory from Cape Canaveral in the latter part of 1960. The

flight profile is such that an altitude of 100 miles and a maximum velocity of 18, 000 ft/sec will be reached in a shallow

(10-20 degrees) re-entry path. The instrumentation consists

of five microwave transmitters, in the L, S, C and X-band frequency ranges, and S and C band receivers. The S and C

band units also serve as the radar beacons while telemetry

data is transmitted on the X band frequencies. Parameters

to be measured include signal attenuation and coherence,

pulse deterioration, and plasma noise generation as a function of altitude and velocity. These results will be compared

with estimated values from modified isentropic calculations

and, also with results from the University of California's

hypersonic wind tunnel tests. Subsequent to the flight test

detailed nonequilibrium real gas calculations will be programmed to provide an exact theoretical comparison. The

radiation patterns of the antennas on the nose cone will be

changed in shape by the plasma sheath. This effect is being simulated experimentally by the use of a lossy artificial

dielectric which has the same propagation characteristics

as the plasma. The realization of an index of refraction of

less than unity was achieved in this artificial dielectric by

the use of a cubic lattice of closely spaced wires. The loss

can be introduced either by loading the wires with lossy elements or by embedding the lattice in a lossy medium. These

same techniques can also be used to simulate plasmas in

radar reflection and diffraction problems.

D-701 Rudkjjrfbing, Mogens (Ole Roemer Observ. , Univ. of Aarhus),

The continuous absorption coefficient of ionized hydrogen at

radio wavelengths. Annales d'Astrophysique, Paris, 22(2):

118-122, March/April 1959. 2 tables, 10 refs. , 21 eqs.

French, English and Russian summaries p. 118. DLC--A general expression for the hydrogen free-free absorption coefficient

256
derived wave mechanically, is shown to agree asymptotically

with a formula based on KRAMER 's classical results in the

limit of long wave lengths and for physical conditions such

as those in the solar corona or in dense nebulae. (Met. Abst.

11. 6-148. ) --Author's abstract.

D-702 Ryan, W. D. (Queen's Univ. , North Ireland) and Harrower, G. A. (Queen's Univ. , Kingston, Ontario), An apparent

solar periodicity in radio star scintillation . Canadian Journal of Physics, Ottawa, 38(6) :883, June 1960. fig. , 2 refs.

DWB, DLC--The radio sources Cassiopeia A, Cygnus A,

Taurus A, and Virgo A were observed at upper culmination

from the Radio Observatory of Queen's University, Kingston,

Ontario, from the beginning of December 1957 to the end of

November 1958. An autocorrelation function was calculated

for the scintillation index for Cygnus A. The results of the

calculation indicate that solar activity contributes directly

to the ionospheric processes responsible for the scintillation

of radio stars, at least at locations in or near the auroral

zone. (Met. Abst. 11. 12-35. )--I. S.

D-703 Rybner, Jorgen and Ungstrup, Emil, L' influence de la zone

d'aurores boreales sur les liaisons radioelectriques . (Effect

of the auroral zone on radio communication. ) Annales des

Telecommunications, Paris, 12(5): 172-173, May 1957. fig.,

3 refs. DLC--Studies of high frequency propagation between

Denmark and western Greenland are reported. Considering

all possible modes of propagation, it is found that the unusually weak field intensities observed may be attributed to D

layer absorption in the auroral zone. (Met. Abst. 9. 5-278. ) --G.T.

D-704 Rydbeck, Olof E. , Chalmers solar eclipse ionospheric expedition 1945 (with experimental results and theoretical investigations of the eclipse effects) . GSteborg, Sweden. Chalmers

Tekniska Hogskola, Handlingar, No. 53, 1946. 42 p. 23

figs. , tables, 17 refs. , 53 eqs. DLC--Automatic and semiautomatic multi frequency equipment was used. The results

discussed show that frequent disturbance of the upper atmosphere and abnormal low layer absorption were quite common;

abnormal E layer reflections appeared almost daily. Ionizing radiation cannot be neglected. Positive proof for the

theory that ultraviolet light from the sun is the primary ionizing force of the E and Fl layers was found. The F2 eclipse

effect is more complex than assumed and a geomagnetic control of the eclipse effect is suggested. Simple formulas for

calculation of E and F minimum solar eclipse electron densities were obtained. --W. N.

257
D-705 Ryle, Martin and Hewish, A. , The effects of the terrestrial

ionosphere on the radio waves from discrete sources in the

galaxy. Royal Astronomical Society, Monthly Notices, 110

(4):381-394, 1950. 3 figs. , 14 refs. Summary in its Geophysical Supplement, 6(2): 138, Oct. 1950. DWB--Observations

of the discrete sources of radio waves in the galaxy have

shown the existence of irregular refraction processes in the

terrestrial ionosphere. These irregularities cause rapid fluctuations in the intensity of the radiation at the ground, while

observations with aerials of high resolving power have shown,

in addition, that the apparent position of a source may vary

irregularly by 2-3 minutes of arc. The incidence of these ir- regularities shows a marked diurnal variation having a maximum at about 01 h 00 m local time. It does not seem possible to account for the irregularities in the ionosphere in

terms of solar emissions and an alternative mechanism is

proposed, based on interception of interstellar matter moving

under the gravitational attraction of the sun. Further experiments may provide information of interest in theories of the

accretion of matter by the sun. (Met. Abst. 5. 11-221.)--

Authors" abstract.

D-706 Ryle, M. (Cavendish Lab. , Cambridge, England), Radio

astronomy. Reports on Progress in Physics, 13:184-246,

1950. 18 figs. , refs. DLC. Translated from Russian in

Uspekhi Fizicheskikh Nauk, Moscow, 46(4): 508 -588, April

1952. 18 figs. , bibliog. p. 586-588. DLC-Experimental

methods are described; then the results of observations of

galactic and solar radiation are presented. Theories covering

these observations are put forward, the aim being a connected

treatment. Particular emphasis is placed on the experimental

and theoretical work, carried out since the war, at the Cavendish Laboratory. (Met. Abst. 9A-158. ) --Physics Abstracts,

No. 23, 1951.

D-707 Ryle, M. and Ratcliffe, J. A. , Radio astronomy. Endeavour,

11(43): 117-125, July 1952. 10 figs. DLC--An analytical

study of the radiation from radio stars (outer space) which is

characterized by the similarity to irregular e. m. f. (radio

noise). No relation between bright radio stars and visible

stars is found. The radio emission from an average radio

star is found to be at least 10^8 times as great as that from

the undisturbed sun. A theory of solar radiation is discussed.

A model chromosphere is presented and a map showing location of radio stars in the Northern Hemisphere is given. (Met.

Abst. 9A-21.)-W. N.

258
D-708 Ryle, M. (Cavendish Laboratory, Cambridge), Radio investigations of the structure of the solar corona. (In: Solar

eclipses and the ionosphere: a symposium. . . ed. by W. J. G.

Beynon and G. M. Brown. London, Pergamon, 1956. p. 246-

252. 4 figs.) DWB--Observations of the solar emission at

meter wavelengths may be used to derive information on the

distribution of electron density and temperature in the undisturbed solar corona. It is necessary to determine at each of

several wavelengths not only the total intensity but also the

distribution of "radio brightness" across the solar disk. These

measurements have been made by observations of the variation of intensity during an eclipse, and more extensively by

using interferometric methods to provide a sufficiently high

resolving power. Using the results of such observations

preliminary models of the solar corona have been derived. An

entirely different method of observation has been used to

study the outermost layers of the solar envelope. In this

method, observations are made of a radio star at different

angular distances from the sun. The results show that as

this angle decreases the apparent singular size of the radio

star increases, due to scattering by irregularities in the electron density. It has been possible to detect this effect out

to distance of 20 RQ , and important deductions about the

electron density in this region can be made. (Met. Abst.

9B-156.) -Author's abstract.

D-709 Ryle, M. (Cavendish Laboratory), Die Entdeckung von

Radiostemen. (Discovery of radio stars. ) Naturwissenschaftliche Rundschau, Stuttgart, 14(4): 133-136, April 1961.

6 figs. DWB, DLC--Radio stars were first discovered by J. S.

Herg in 1948 with the aid of a 5 m radar; directed toward gaseous clouds in constellation Cygnus. By means of an interferometric radio telescope, whose operation is described with

the aid of a diagram, it was shown that the radiation source

in Cygnus had a surface brightness several thousand times

greater than the brightness of the galactic system. By means

of precise observations made by F. G. Smith in Australia (1950)

it was possible to determine exact positions with an accuracy

of 1 x 1/4 arc minutes, and by means of the 200 inch Palmar

telescope Boade and Minkawaki (1951) established the fact

that the radio source in the constellation Cassiopeia was the

remains of a super nova. The radio source in Cygnus was an

extragalactic cloud about 500, 000, 000 light years away. A

comparison of observations of neighboring galactic systems

with those at varying distances, such as those provided by

radar observations of extragalactic systems, enables a determination of the state of the cosmos at different times. From

sufficient observations of radio stars it would be possible to

determine whether the universe originated some 10 billion

years ago or whether it is a permanently invariable universe.

259
Out of 500 accurately recorded positions of radio stars only

27 could be perceived optically. Eight of these are within

our own galactic system and are remainders of super novae.

Eleven belong to neighboring galaxies, a few of which possess a million fold emission capacity; some of these are double sources and may be instances of collision of two galaxies. Most of the radio stars belong to powerful and distant extragalactic sources. --I. L. D.

D-710 Sadler, D. H. , The place of astronomy in navigation. Institute of Navigation, London, Journal, 9(1): 1-10, Jan. 1956.

5 figs. DWB--Recent applications of astronomy to navigation

include the Pfund sky compass, which uses the polarization

of light by the atmosphere to indicate the position of the sun

when obscured by clouds or below the horizon, and radioastronomy. Waves from about 1 cm to 30 rmare received

from the sun. Radio sextants of practicable size using wavelengths of 1. 9 cm and 8. 7 mm are illustrated. Lunar tracking

has been accomplished experimentally. Vertical reference is

possible by 3 Geiger counters receiving cosmic rays. These

projects will be aided by the International Geophysical Year.

(Met. Abst. 7. 7-21. )-C.E. P. B.

D-711 Saha, A. K. ; Ray, S. ; Datta, S. et al. , Ionospheric observations during the solar eclipse of June 20, 1955. Science

and Culture, Calcutta, 21(8):475-477, Feb. 1956. 4 figs.

,

2 refs. DLC --Ionospheric records made at the Ionosphere

Field Station at Haringhata (22. 9°N, 88. 5°E; Geomagnetic

latitude 12. 5 N, 28 miles NE of Calcutta) where the eclipse

of June 20, 1955 was 0. 67 total and the duration 2& hours,

are discussed with respect to E, Sporadic E, Fl and F2 layer

variations. E region ionization dropped to 35% of average of

control days (1 month on either side of eclipse), about 30 min

before eclipse maximum. Maximum drop could not be recorded because of Es ionization. No change in fEs values could

be detected. Fl layer showed a drop to 20% of control day,

8 minutes after maximum observation at ground. F2 ionization was higher than average before eclipse, started to drop

1

{6. hours before eclipse, dropped by ca. 31% 20 minutes after

eclipse maximum at ground, and took 346 hours to recover. Theory involves solar particles 1500-2000 km/sec. (Met.

Abst. 8. 5-183. )-M.R.

D-712 Sarada, K. A. (Nat. Physical Lab. , New Delhi, India),

Sudden cosmic noise absorption associated with the solar

event of March 23, 1958. Journal of Atmospheric and Terrestrial Physics, London, 13(1/2): 192- 194, Dec. 1958. 3 figs.

,

table, 2 refs. , 3 eqs. DLC--A large absorption effect (SCA)

was observed in the records of cosmic radio noise at 30 Mc/s

obtained at the National Physical Laboratory, New Delhi, on

260
March 23, 1958. Unusual features of this effect were: indication of an excess absorption some thirty-five times the

normal value and a residual radiation attributable to the thermal radiation of the lower ionosphere. It is possible that a substantial portion of attenuation was caused by processes

other than collisional absorption. (Met. Abst. 12. 6-161. ) -O. T.

D-713 Scheffler, H. (Potsdam), Zur Berucksichtigunq der Mehrfachstreuunq in der Theorie der Szintillation optischer und

radiofrequenter Strahlung. (Consideration of multiple scattering in the scintillation theory of optical and radio frequency radiation. ) Astronomische Nachrichten, Berlin, 284(1):

21-23, July 1957. 12 refs. , 7 eqs. DLC- -Connections between recent theories of ELLISON, OBUKHOV, KELLER, FEJER

and the author on the scattering of electromagnetic waves in a medium with statistically distributed refractive index variations are discussed in regard to the consideration of multiple

scattering. (Met. Abst. 12. 1-105. )--Transl. of author's

abstract.

D-714 Schiffmacher, E. R. , Investigation of solar radio frequency

at USAF Upper Air Research Observatory, Sunspot. New

Mexico. Cornell Univ. School of Electrical Engineering, Contract AF 19(604) -73, Final report; Research Report EE 299,

July 1, 1956. 24 p. photo. --Radio Observatory at Sacramento Peak, New Mexico, and antennas for 3 wavelengths of

radiation are shown in photograph. Work from 1948-1955

under 2 contracts are reviewed and summaries given for 12

reports or papers issued under these contracts. Optical effects observed in vicinity were compared with enhanced radio

frequency radiations from sun. Radio astronomy technical re- ports and bibliographies prepared at Ithica, N. Y. , in connection with theoretical work and analysis of observations, are also summarized. It was. found that 200 Mc/sec was the

most useful frequency for solar radio observations. (Met.

Abst. 9A-133.)--M.R.

D-715 Schilling, G. F. and Fergusson, E. S. (both, Astrophysical

Obs. , Smithsonian Inst. ), Soviet orbit predictions and orbital information for U. S. S. R. satellites 1957 Alpha one. Alpha

two and Beta. Smithsonian Institution. Astrophysical Observatory, IGY Project No. 30. 10, Special Report, No. 5, Dec.

4, 1957. 51 p. mostly tables. 4 refs. Also issued in "edited form" as Smithsonian Contributions to Astrophysics, Wash.,

D. C. , 2(10): 219-244, 1958. DWB, DLC-The Soviet predictions on positions and times of passage overhead of U. S. S. R.

satellites (1957): Alpha one (carrier rocket). Alpha 2 (Sputnik) launched Oct. 4, 1957, and Beta, the instrumented rocket launched Nov. 3, 1957, as issued from Oct. 23, 1957 to

261
Dec. 6, 1957 in Soviet newspapers and radio broadcasts.

Other technical information released during this period is

appended and results tabulated. (Met. Abst. 10.5-112.)--

M.R.

// D-716 Schindelhauer, F. , Uber die Richtung atmospharischer

Stoningen. (Direction of sferics.) Jahrbuch der Drahtlosen

Telegraphie und Telephonie, 22(4): 163- 167, Oct. 1923. fig. , ref. , eqs. DLC- -Observations conducted at the Potsdam Observatory in March 1922 by means of a rotary frame operating

within 21, 000 m wavelength, showed that the NS direction of

sferics was remarkably constant and independent of the

weather conditions. The diurnal variation observed indicated solar relation. Direction during night hours showed

no distinct trend. The maximum intensity was at 18 h with

minimum at 8 h. (Met. Abst. 4K-27. )«W. N.

D-717 Schmelovsky, Karl Heinz; Klinker, Ludwig and Knuth. Robert

(all, Obs. for Ionosphere Research, Kuhlungsborn), Uber

die Elektronenkonzentration in der ausseren Ionosphere nach

Untersuchungen des Faraday-Fadings am Satelliten 1958 Sa.. (Electron concentration in the upper atmosphere from investigations of the Faraday-fading of 1958 oz satellite. ) Beitrage

zur Geophysik, Leipzig, 68(6):321-341, 1959. 10 figs.

,

table, 10 refs. , 13 eqs. German and English summaries p.

321. DWB, DLC--Methods for evaluating the Faraday fading

of satellite signals are derived from the APPLETON-HARTREE

formula. Reliable values for the total electron number can

only be obtained by an iterative, approximation based on a

sufficient number of observations. A height-electron-density

distribution for the region between the F2 layer and 1200 km

is determined from 135 observations during the summer 1958.

Between 500 to 900 km there is a decrease in electron density with exp (-aH); a = 2. 5 X 10"3 km "1. The total electron content up to 1200 km is 3. 6 X 1017 m-2. about 70% of

this amount belong to the region above F2 layer maximum.

About 2/3 of the diurnal variation in total electron number is

produced below the F2 layer maximum. During magnetic and

ionospheric disturbances there is a decrease of total electron

number. (Met. Abst. 11. 12-376. )--Authors' abstract

D-718 Schmidt, H. , Planetarische Radiostrahlunq. (Radio emission from planets. ) Die Sterne, Leipzig, 36(3/4) :81-83,

March/April 1960. DLC --In agreement with the 101st session of the American Astronomical Society a symposium was

organized in December 1958 at Gainesville. The author

shows the observations made in the field of radio astronomy

by K.L.FRANKLIN, B.BWIKE, H.TATEL, T.D.CARRand

others. From the results of various research works the conclusion was reached that besides the sun, only Jupiter may

262
be considered as a radio source; Venus, Saturn and the

cornets need a more developed research. The author gives

some results of measurements: (Venus) by MEYER—3. 15 cm

and 3. 4 cm wave; (Jupiter) by MACCLAIN and SLOANAKER —10. 3 cm. Observations of Saturn in 1958 have been without results. (Met. Abst. 11. 12-63. )--A. V.

D-719 Schwentek, Heinrich, Bestimmung eines Kennwertes fur die

Absorption der Ionosphare aus einer. automatische-statistischen Analyse von Feldstarkereoristrierunqen . (Determination

of an ionospheric absorption coefficient by means of automatic-statistical analysis, of field strength recordings.)

Archiv der Elektrischen Ubertragung, Stuttgart, 12(7) :3Q1-

308, July 1958. 11 figs. , 15 refs. , 14 eqs. DLC--A simple

method is described by which the nondeviative absorption of

the ionosphere can be determined continuously by field

strength measurements at oblique incidence. The conditions

of a suitable transmission path are discussed. An analysis

of the field strength frequency distribution measured by a

statistical counter renders possible the separation of the

main transmission paths from each other. Thus absorption

values for hourly intervals can be determined immediately.

For this purpose the absorption values are reduced to vertical incidence. Furthermore the state of the ionosphere may

be derived from the distributions. Thus the mean reflection

coefficient of the Es layer at night as well as its frequency

are immediately obtained. For the delayed diurnal variation

of absorption dependent on the sun's zenith angle a simple

formula is suggested. (Met. Abst. 11E-138. ) --Author's

abstract.

D-720 Scott, James C. W. (Radio Phy. Lab. , Def. Res. Bd. , Ottawa),

The solar control of the E and F 1 layers at high latitudes.

Journal of Geophysical Research, 57(3):369-386, Sept. 1952.

19 figs. , 3 refs. DWB--The monthly mean critical frequencies

of the E and Fl layers at high latitudes are shown to vary diurnally with solar angle according to a modified Chapman law.

The seasonal, latitude, and solar cycle dependence of the E

layer sensitivity to solar angle and the sub-solar frequency

are measured. In the auroral zone, the sensibility of the E

layer to solar angle is shown to be very low, but to the north

of the zone it is found to have the theoretical Chapman value.

(Met. Abst. 6D-136. )--Author's abstract.

D-721 Seddon, J.Carl (U. S. Naval Res. Lab. , Wash. , D. C. ), Propagation measurements in the ionosphere with the aid of rockets. Journal of Geophysical Research, Wash. , D. C. , 58(3):

323-335, Sept. 1953. 10 figs. , 7 refs. , 11 eqs. DWB--

Daytime measurements of electron density, ion density, electron collision frequency, and earth's magnetic field in the

263
ionosphere were made during V-2 rocket flights at the White

Sands Proving Ground, New Mexico. Two CW harmonically

related frequencies were radiated from the rocket to two

ground stations to obtain measurements of the ordinary and

extraordinary indices of refraction in the region around the

rocket. The results for one flight show an ion layer with a maximum of 5 X 10° ions/cc and a small electron layer with

a maximum of 7500 el/cc just below the El layer. On a September day the Fl layer remained dense up to the E2

layer, while on a January day the density apparently decreased above the Fl layer maximum to much lower values.

It is shown that the Lorentz polarization term should not be

used in the E layer at 4 Mc. (Met. Abst. 6. 1-62. )--Author's

abstract.

D-722 Seddon, J. C. (Naval Res. Lab. , Wash. , 25, D. C. ), Propagation measurements in the ionosphere with the aid of rockets . (In: Boyd, R.L.F. ; Seaton, M.J. and Massey, H. S. W.(eds. ),

Rocket exploration of the upper atmosphere. London, Pergamon, 1954. p. 214-222. 10 figs. , 5 refs. ) DWB--The upper

atmosphere has been measured by the Naval Research Laboratory since 1946. Earlier methods used for measuring electron densities and the basic experiments performed are discussed. In 1949 it was observed that the electron density

did not drop much above the El layer maximum. This caused

the vertical heights of reflection to be far greater than the

actual height of the reflection. A method of determining the

harmonic frequency system is described and is considered

the best means of probing the secrets of the ionosphere when

used with high altitude vehicles such as the V-2 rockets.

(Met. Abst. 11E-141.)-N.N.

D-723 Seddon, J. C. , Rocket investigations of the ionosphere by

radio propagation method. U. S. Naval Research Laboratory,

Upper Atmosphere Research Report, No. 22; NRL Report

4304, March 1, 1954. 37 p. figs. , tables, 9 refs. , eqs.

DWB--Daytime measurements of electron density, ion density,

electron collision frequency, mean molecular cross section,

and earth's magnetic field during V-2 rocket flights at the

White Sands Proving Ground, New Mexico, were obtained on

March 7, 1947, Jan. 22, 1948, and Sept. 29, 1949. In each

case a 4. 274 Mc signal and its 5th harmonic were radiated

from the rocket to receiving stations on the ground to obtain

measurements of the. ordinary and extraordinary indices of re- fraction of the region around the rocket. The results of one

flight show an ion layer with a maximum of 5 X 10°* ions/cc

and a small electron layer with a maximum of 7500 el/cc just

below the El layer. On a September day the El layer remained dense up to the E2 layer, while on a January day the density apparently decreased above the El layer maximum to

2S4
much lower values. It is shown that the Lorentz polarization

term should not be used in E layer computations at 4 Mc. A

detailed explanation of the data analysis methods is included

in the appendixes. Extensive calculations using the general

Appleton-Hartree formula have been made at 4. 274 Mc and

some of the results are shown for various collision frequencies, using the value of the magnetic field at 100 km above

the White Sands Proving Ground, New Mexico. (Met. Abst.

6D-265. )- -Author's abstract.

D-724 Seddon, J. C. (Rocket Sonde Branch, U. S. Naval Res. Lab. ),

High electron density gradients in the ionosphere as observed

with rockets. AGARDograph, Paris, No. 34:171-181, Sept.

1958. 5 figs., 2 tables, 7 refs. DWB (629. 1323 N834a)~

Many daytime measurements of electron density profiles with

rockets have been made during the condition known as "sporadic E". In all cases, it was found to be a high electron

density gradient region covering in general a radius in excess

of 50 km. Gradients as large as 10° el/cc per km have been

observed. Various characteristics of sporadic E, such as

horizontal variability, thickness, and maximum electron densities are briefly discussed. Evidence of many other large

electron density gradients between 66 and 2C0 km is presented. One such gradient is always found to be present near

the mesopause. The others are variable in occurrence and

altitude, except for a strong tendency for E region gradients

to occur at particular altitudes separated by about one scale

height. One night flight at Fort Churchill, Manitoba, Canada is discussed where two sporadic E regions existed. One

of these, at 98 km, had a characteristic never before observed, of the large gradient being on top side. Evidence is presented that shows that a spread F condition existed above

190 km and that it probably consisted of many irregular, turbulent high gradient regions. (Met. Abst. 11D-128. )--

Author's abstract.

D-725 Seddon, J. C. and Jackson, J. E. , Rocket studies of the Arctic ionosphere. American Geophysical Union, Transactions,

40(l):63-65, March 1959. DWB-Three rocket flights furnished strong evidence that a polar blackout is due to an abnormal number of free electrons in the D region of the ionosphere,

and that moving electric charges play an important role in

this phenomenon. The polar blackout seems to involve little

change in the E and F regions of the daytime ionosphere. The

daytime electron density in this region of the ionosphere is

similar to that in lower latitudes. The electron collision frequency with neutral particles may be 1/3 or 1/4 that previously estimated. Radio wave absorption in the Arctic ionosphere

varies from extremely high to extremely low values. (Met.

Abst. 11. 12-362. )-E. Z. S.

265
D-726 Seddon, J. C. (Nat'l. Aeronautics and Space Admin. ), Rocket

observations of high electron density gradients in the ionosphere. American Geophysical Union, Transactions, 41(1):113-

118, March 1960. 4 figs. , 2 tables. DWB, DLC-- A discussion of high electron density gradients and their significance

in terms of ionospheric conditions. For the purpose the U. S.

Naval Research Laboratory launched a number of rockets at

White Sands, New Mexico and Fort Churchill, Canada. In all

ionospheric regions penetrated by the rockets, high electron

density gradients were found. In the D region a high gradient

was almost always present near the mesopause. In the £ re- gion a slightly above high gradients were associated with sporadic E at various levels. They appeared related to the distribution of spread F in the F region. (Met. Abst. 11. 12-363.)--

I.S.

D-727 Seddon, J. C. (Goddard Space Flight Center), Summary of

rocket and satellite observations related to the ionosphere . U. S. National Aeronautics and Space Administration, Technical

Note D-667, Jan. 1961. 22 p. 5 figs. , 114 refs. , 5 eqs.

Also issued as: National Research Council, Wash. , D. C. , Publication No. 880:233-249, 1961. DWB, DLC--New knowledge

relating to the earth's ionosphere in the past 3 yrs by rocket

and satellite methods is reviewed. Measurements of electron

densities up to and above the F2 maximum, columnar electron

densities, electron density gradients, sporadic E, and spread

F are discussed. Other parameters important to the formation

of the ionosphere are also briefly discussed. An extensive

bibliography on these subjects are given. --NASA Abst. TN D667.

D-728 Seddon, J. C. and Jackson, J. E. (both, U.S.A.), Summary of

progress made in ionospheric research using rockets and satellites during the IGY. (In: International Scientific Radio Union.

IGY Committee, Some ionospheric results obtained during the

IGY. Amsterdam, Elsevier, 1961. p. 388-390.) DWB, DLC--

An unusual large number of free electrons in the D region re - sponsible for polar blackouts by absorbing radio waves in the

broadcast range was recorded by Aerobee-Hi rockets. This ex- ceptionally high ionization of the D region provided unique

conditions for the measurements of the electron collision frequencies with neutral particles. Rocket results at sunspot

maximum indicated an electron density gradient of 10^ electrons /cc/km in the E and F2 regions. The Russian rocket and

satellite data showed high electron density at 1000 km and

their data projected to higher altitudes concur with whistler

measurements in U. S. (Met. Abst. unpub. )--S. N.

266
D-729 Sen Gupta, Prabhat K. and Mitra, S. N. , Corpuscular eclipse

in the F2 layer and its association with solar flares and M re- gions. Nature, London, 173(4409) :814-816, May 1, 1954. fig.,

20 refs. DWB--Eclipse of a solar corpuscular stream about 2

hrs before optical eclipse shows that fast corpuscles have

velocities about 1600 km/s, but fade outs are rarely connected

with solar flares. M storms may be due to corpuscles taking

1-3 days to reach earth according to intensity. S. N. MITRA

found two corpuscular eclipses 2£ and 5 hrs before optical

eclipse of Feb. 25, 1952, indicating speeds of 1300 and 640

km/s. Magnetic and ionospheric disturbances on Feb. 23-25

are attributed to corpuscular streams associated with M regions.

(Met. Abst. 5. 8-99. )--C.E. P. B.

D-730 Sedra, R.N. and Hazzaa, I. B. (both. Faculty of Science,

Cairo Univ. , Giza, Egypt), Effect of radiation from solar

flares on the ionosphere and the earth's magnetic field. Physical Review, N.Y. , 99(4): 1070-1072, Aug. 15, 1955. 3 figs.,

table, 5 refs. , 5 eqs. Also: Agy, Vaughn, Ionospheric effects produced by solar flare radiation. Ibid. , 102(3) :917,

May 1, 1957. 3 refs. DLC--Variation in the earth's magnetic

field and the corresponding variations in the ionic density of

the Fl layer due to solar flares are recorded. The value of the

intensity of ultraviolet radiation before it enters the atmosphere is obtained. The constant relating the ionic density and

the accompanying magnetic variation is also estimated. AGY

pointed out that UV radiation from solar flares does not produce changes in ion density of E and Fl layers but rather at

K 100 km. Other deficiencies are noted. (Met. Abst. 8. 10-

132. )- -Authors' abstract, M. R.

D-731 Seeger, Charles L. (Cornell Univ. ), Observations of the

variable 205 Mc radiation of Cygnus A. Cornell Univ. School

of Electrical Engineering, Contract N6onr-264, T. O. 6, NR

077-321, Radio Astronomy Report, No. 8, Oct. 1, 1950. 33 p.

5 tables, 10 figs. , 8 refs. DWB--The first evidence of any

large variation in the 205 Mc galactic radio frequency from the

Cygnus region, was obtained on the night of Oct. 18, 1949.

Results for some 200 nightly observations of two to ten hours

duration, contradict the results as obtained by BOLTON and

STANLEY insofar as the variation of intensity of radiation is

concerned. The chief cause of variation in the flux of the incoming radiation from outer space seems to be traceable to

scattering by random inhomogeneities in the earth's atmosphere (ionosphere). (Met. Abst. 9A-12. )--W. N.

267
D-732 Seeger, C.L. ; Stumpers, F.L.H. M. and Hurck, N. van,

A 75 cm receiver for radio astronomy and some observational

results . Philips Technical Review, Eindhoven, Netherlands,

21(ll):317-333, Sept. 27, 1960. 18 figs. , 16 refs. , 5 eqs.

DLC (TK1. P5) --Description of a simple, stable, and sensitive

receiver for the frequency range from 200 to 500 Mc/s (150 to

60 cm) possessing a very low noise factor which makes possible accurate observations of the very weak radio waves re- ceived from estraterrestrial sources. The receiver operates

on the superheterodyne principle, with an intermediate frequency of 50 Mc/s. Various radio astronomical observations are described that have been made with this receiver, particularly

in conjunction with the 25 m parabolic reflector of the radio

observatory at Dwingeloo. The isophot chart of the sky drawn

from the observations made with this radio telescope, and re- produced in this article, provides the most detailed information

at present available on the structure of our Galaxy, measured

at 400 Mc/s. The article is well issultrated. --E.Z. S.

D-733 Sen, Hari K. (U.S. Nat'l. Bureau of Standards, Wash. , D. C),

Space charge wave amplification in a shock front and the fine

structure of solar radio noise. Australian Journal of Physics,

Melbourne, 7(l):30-35, March 1954. 2 figs. , 11 refs. , 6 eqs.

DWB--The Mott-Smith (1951) interpolation method gives a nonMaxwellian velocity distribution for the particles in a shock

front. The dispersion equation corresponding to the non-Maxwellian distribution is derived by VLASOV's (1945) formula.

The roots of the dispersion equation indicate frequency bandwidths of space charge wave amplification that decrease with

the shock strength. It is suggested, in agreement with

DENISSE and ROCARD (1951), that the storm bursts of narrow

bandwidth originating in shock fronts constitute the elementary

fine structure components of solar radio noise bursts. (Met.

Abst. 9A-63.) --Author's abstract.

D-734 Sen, S. N. , Total solar eclipse of Feb. 1952. Science and

Culture, Calcutta, 18(l):22-25, July 1952. 4 figs. , map.

DWB--Brief report on observation of the solar eclipse in Feb.

1952 conducted at Khartoum, Sudan, by about 60 scientists

belonging to 17 separate expeditions from Europe and the U. S.

Results obtained in solar radio noise and chromospheric temperature measurement, in studying the corona and in geodetical observation are summed up. Photographs showing equipment used by U. S. scientists are reproduced from various

American journals. Achievements of French amateur astronomers are mentioned. (Met. Abst. 4. 5-250. )--G. T.

268
D-735 Sengupta, Dipak L. (Univ. Michigan), Electrical conductivity of a partially ionized gas. Institute of Radio Engineers,

N.Y., Proceedings, 49(12): 1872- 1876, Dec. 1961. 8 refs.

39 eqs. DLC--The electrical conductivity of a low density and

partially ionized gas where both electron -neutral particle and

Coulomb type collisions play important roles is discussed.

The effects of inelastic collisions and a steady magnetic field are not considered. We assume that the ionized gas is perturbed by a weak electric field, and obtain the velocity distribution function for the electrons by solving the Boltzmann

equation; the collision between neutral and charged particles

is accounted for by the hard sphere model for the particles,

while the collision between the charge particles is taken care

of by the Fokker-Planck terms. Explicit expressions for ac

and dc conductivity are given for various cases. To the extent that the assumptions made for the collision models are

valid, the expressions for conductivity given here are quite

general and can be used for any degree of ionization. (Met.

Abst. unpub.) --Author's abstract.

D-736 Senior, T.B. A. and Siegel, K. M. (both, Univ. of Michigan,

Ann Arbor, Mich. ), Radar reflection characteristics of the

moon. (In: Paris Symposium on Radio Astronomy, July-Aug.

1958, (Proceedings), pub. Stanford Univ. Press, 1959. p. 29-

46. 3 figs. , 13 refs. , 9 eqs. DLC—This paper presents a theory based on the concept of a "quasi-smooth" scattering

mechanism. The theory was developed from a study of many

sets of experimental data and it is thought that the pulse

shape and power returns can be satisfactorily explained on

this basis, as can their polarization dependence. Some of

the results explained can be applied to the design of communication systems that employ scattering from the moon. The

moon can be used as a parasitic antenna to provide communication between widely separated points on the earth's surface.

This aspect is briefly discussed and reasons for advocating

the use of the 3 cm band for this purpose are given. The relevant parameters of such a system is presented. --E. Z. S.

D-737 Senior, T.B. A. and Siegel, K. M. (Univ. Michigan). A theory

of radar scattering by the moon. U. S. National Bureau of Standards, Journal of Research, Sec. D, (Radio Propagation), 64(3):

217-229, May/June 1960. 5 figs. , table, 25 refs. , 17 eqs.

DLC, DWB--A theory is described in which the moon is regarded as a "quasi-smooth" scatterer at radar frequencies. A scattered pulse is then composed of a number of individual returns

each of which is provided by a single scattering area. In this

manner it is possible to account for all major features of the

pulse, and the evidence in favor of the theory is presented.

From a study of the measured power received at different frequencies, it is shown that the scattering area nearest to the

269
earth is the source of a specular return, and it is then possible to obtain information about the material of which the

area is composed. The electromagnetic constants are derived

and their significance discussed. (Met. Abst. unpub. )--

Authors' abstract.

D-738 Setty, C. S. G. K. (Dept. Physics, Cent. Coll. , Bangalore),

Eclipse effects on the Fl layer observed at Cambridge on June

30, 1954. Journal of Atmospheric and Terrestrial Physics,

London, 19(2):95-101, Oct. 1960. 2 figs. , 2 tables, 4 refs.

,

4 eqs. DLC--A study is made of the solar eclipse effects on

the Fl layer, observed at Cambridge on June 30, 1954, using

the critical frequency data following the method developed by

C.M.MINNIS. The h'(F) records were made during the period

June 26 to July 5, 1954 using a panoramic ionosphere recorder.

Only a lower limit can be set for X the recombination coefficient in the Fl layer and a value of 8 X 10-9 i s not unsuitable.

The major part of the radiation causing the Fl layer ionization

is almost uniformly distributed over the entire visible disc of

the sun, except for some west limb brightening to explain a discontinuity in the eclipse variation of the critical frequency,

a source of radiation 10% of the whole will have to be assumed

to lie beyond the visible disc of the sun. (Met. Abst. 12. 4-

108. )- -Author's abstract.

D-739 Shain, C. A. , Galactic radiation at 18.3 Mc/s . Australian

Journal of Scientific Research, Ser. A, Physical Sciences,

4(3):258-267, Sept. 1951. 7 figs. , 15 refs. , 2 eqs. MH-BH

--Observations are described of galactic radiation at a frequency of 18. 3 Mc/s over a zone of the sky centered on declination -34 . The results, expressed as equivalent temperatures,

are compared with the distribution of intensity at 100 Mc/s. It is found that the temperatures are consistently much higher at

18. 3 Mc/s than at 100 Mc/s but the observed ratio of maximum

to minimum at 18. 3 Mc/s is less than would have been obtained at 100 Mc/s using an aerial with the same directional diagram. The observations are consistent with the hypothesis

that contours of equal equivalent temperature over the sky are

of similar shape on the two frequencies. Peaks in the intensity

distribution are observed which appear to be due to discrete

sources. The observations give information concerning the

attenuation of radiation passing through the ionosphere. It is

found that F region absorption is higher near the critical frequency than expected, and that E region absorption is lower

than expected. It is found that the collision frequency at the

height of maximum ionization of the E region is not greater

than 10^*sec"l, and is probably less. For the equipment used,

the limit of sensitivity for the reception of radio signals was

generally set by galactic noise. (Met. Abst. 4.9-112.)--

Author's abstract.

270
D-740 Shain, C. A. and Higgins, C. S. , Observations of the general

background and discrete sources of 18. 3 Mc/s cosmic noise.

Australian Journal of Physics, 7(1): 130-149, March 1954. 11

figs. , 2 tables, 12 refs. DLC--A survey of a broad strip of

the sky, centered on Dec. —32 , has been made at a frequency of 18. 3 Mc/s using an aerial with an overall beam width to a half power of 17 . Previous results concerning the background distribution of brightness have been confirmed and 37

discrete sources have been detected. The distribution of

these sources shows some galactic concentration; it becomes

homogeneous if sources within 18 of the galactic plane are excluded. From observations of source scintillations, it is

concluded that some of the discrete sources have angular

sizes of the order of 1 . No correlation was found between

the occurrence of scintillations and published ionospheric

data, but the observations are consistent with an origin of

the scintillations in irregularities, of dimensions about 4 km,

at a height of about 500 km. (Met. Abst. 9A-65. )- -Authors'

abstract.

D-741 Shain, C.A. and Mitra, A. P. , Effects of solar flares on the

absorption of 18. 3 Mc/s cosmic noise. Journal of Atmospheric and Terrestrial Physics, 5(5-6) :316-328, Nov. 1954.

7 figs. , 3 tables, 10 refs. DWB--Observations of abnormal

ionospheric absorption in New South Wales showed sudden

increases coinciding with SID's and solar flares. "An increase of 1 db in absorption on 18. 3 Mc/s radiation passing

once through the ionosphere is probably associated with a sudden phase anomaly of size about 200 at 16 kc/s. Such a relationship is incompatible with a D region of the simple

Chapman type or one of the 'exhaustion region' type. About

30 hrs after certain solar flares of Class 3 the absorption of

cosmic noise increased, the increase lasting for periods of

the order of 10 hrs. Magnetic storms did not follow until

some time later, and at the time of the abnormally high attenuation there were no outstanding peculiarities in magnetic re- cords. It is uncertain whether the excess attenuation occurs

within the ionosphere or well away from the earth. " (Met.

Abst. 9A-64. )--From authors' abstract.

D-742 Shain, C. A. , Location on Jupiter of a source of radio noise.

Nature, London, 176(4487) :836-837, Oct. 29, 1955. 2 figs.

,

2 refs. DWB--Radio noise on 18. 3 Mc/s on Jupiter is traced

to a disturbance at the boundary between the South Temperate

Zone and the South Temperate Belt, possibly originating in

electrical discharges. (Met. Abst. 9A-92. )-C. E. P. B.

271
D-743 Shain, C.A. , Changes in the absorption of cosmic noise

observed during two ionospheric disturbances. Journal of

Atmospheric and Terrestrial Physics, 7(6):347-348, Dec.

1955. fig. , 3 refs. DWB—Observed total absorption at

Hornsby (34 S, 151T!) compares with foF2 at Brisbane and

Canberra on Aug. 19-21 and Nov. 23-25, 1950. (Met.

Abst. 11E-145.)--C.E.P.B.

D-744 Shain, C.A. (Div. of Radiophysics, C.S.I. R. O. , Univ.

Grounds, Sydney), 18. 3 Mc/s radiation from Jupiter. Australian Journal of Physics, Melbourne, 9(l):61-73, March

1956. 7 figs. , 7 refs. DLC-BURKE and FRANKLIN' s discovery of radio emission from Jupiter has been confirmed.

Examination of old records has shown that in 1950-51 the

radiation came in groups of bursts of very high intensity.

Bursts have duration of the order of a minute or less;

groups of an hour. Because of the remarkably close relation between active periods and the period of rotation of

Jupiter, it is inferred that the source at the time was very

localized. Its identification with a visual disturbance in

the South Temperate Belt is very probable. It is pointed

out that occultation by Jupiter's satellites may help to

locate the sources of radiation, both in position and in

height relative to the visible surface, and that Jupiter

radiation should be a valuable tool for studying the outer

regions of the solar corona. (Met. Abst. 9A-172. ^-Author's abstract.

D-745 Shain, C.A. and Higgins, C.S. (both, Div. of Radiophysics, C.S. I.R.O. , Univ. Grounds, Chippendale, N. S. W. ),

Location of the sources of 19 Mc/s solar bursts . Australian

Journal of Physics, Melbourne, 12(4): 357-368, Dec. 1959.

5 figs. , 3 tables, 11 refs. DLC--By using large aerials in a new way, it has been possible to locate, with considerable accuracy, the sources of 19 Mc/s bursts. The positions of these sources have been correlated with the positions of optically active regions associated with them, and

the radial distances of the radio sources from the center of

the Sun have been deduced. In 1950-1951, 18. 3 Mc/s

bursts came from sources at a radial distance estimated as

3.4 R ; more reliable data in 1957 indicated that the sources

of 19. 7 Mc/s bursts were at a radial distance of 2. 9 RQ

. It is thought that these measurements give the distances of the

fundamental plasma levels in coronal streamers. (Met. Abst.

11. 12-58. ) -Authors' abstract.

D-746 Shibata, Hisashi, On the "minimum loss operation time" for

short wave communication. Japan. Radio Research Laboratories, Tokyo, Review, 4(15):112-117, April 1958. 2 figs. , 272
32 eqs. In Japanese; English summary p. 112. DLC--At

the present stage of the "radio propagation prediction ser- vice" we have usually the median MUF and the median LUF.

These values are worthy of consideration in an attempt to

foresee the ionospheric conditions and are of cardinal importance from the theoretical point of view. Nevertheless,

in the case of communication in practice these are not ac- cepted as values very suitable for the purpose of determining the operation time. In this paper a method of defining

the optimum operation time will be shown, the probability

of communication being taken into consideration. The

"minimum loss operation time" defined here is only one of

the concepts based on wider considerations which will be

shown in Appendix. In Appendix we show some applications of the criteria used very often in the statistical

theory and in the communication theory for the problem of

the radio disturbance warning service.

Shkarofsky, I. P. (RCA Victor Co. , Ltd. , Montreal, Can. ),

Generalized Appleton-Hartree equation for any degree of

ionization and application to the ionosphere. Institute of

Radio Engineers, N. Y. , Proceedings, 49(12): 1857-1871,

Dec. 1961. 12 figs. , table, 35 refs. , 68 eqs. DLC--A

generalized Appleton-Hartree equation is derived, applicable to any variation of electron collision frequency with

electron speed and any degree of ionization. Regions of

the parameters were simplification occurs are given. Results are shown for the ionosphere (60 to 320 km) and compared with experimental data. Good agreement is obtained

for the D layer. Experimental data for the E layer can also

be explained by assuming an electron temperature several

times the gas temperature. This is consistent with rocket

data and a measurement by Sputnik III. It. is shown that

the classic Appleton-Hartree equation should be applicable

with no corrections necessary for the F2 layer, provided the

collision frequency is averaged appropriately. (Met. Abst.

unpub. ) --Author's abstract.

Shkarofsky, I. P. ; Johnston, T. W. and Bachynski, M.P.

(RCA. Montreal, Canada), Relaxation phenomena in shock

fronts . (A review). Planetary and Space Science, N. Y. , 6:

221, June 1961. Abstract only. The paper was presented at

the Plasma Sheath Symposium, Boston, Mass. , Dec. 7-9,

1959. --For aerodynamic phenomena occurring at temperatures

in excess of 1000 K, a great number of collisions between

the constituent particles of a gas are required in order that

thermal equilibrium be established. Under these conditions,

relaxation times can be associated with the distribution of

the internal energy of the gas into the various energy states.

This paper reviev/s the phenomena occurring in a shock front

from the start of the shock to the point of thermal equilibrium

273
behind the shock. Chemical reactions at high velocities,

temperature variations across a shock front, mechanisms of

energy transfer and effects of air flow rate on relaxation are considered. A comparison of a plasma set up by a hot gas

and one created by a gas discharge is given. The distribution of energy into translational, rotational and electronic

states, as well as dissociation and ionization, are discussed

in detail. Some regard is given to relaxation rates, collision

processes, ionization onset point and radiative relaxation.

D-749 Shklovskii, I. S. , Radioastronomiia . (Radioastronomy.

)

Moscow, Gos. Izdat. Tekhniko-Teoreticheskoi Lit. , 1953.

214 p. 96 figs. (incl. photos), foot-refs. DLC--A popular

edition (10, 000 copies published) giving the latest in the

basic physics of radio propagation theory, including details

as to its penetration through the earth's atmosphere-ionosphere; methods of radioastronomical investigation (radiotelescopes of various types illustrated); radio radiation from the

sun (observations made from ship "Griboedov" during eclipse

of May 20, 1947 in Bahia, Brazil), and from solar eruptions,

from the moon, the galaxies (62. 5, 150, 163, 185 and 300

cm); hydrogen radiation of 21 cm, radio stars, cosmic rays

and radio waves from galaxies, radiogalaxies and, finally,

radiolocation astronomy. (Met. Abst. 7. 6-5. )--M. R.

D-750 Shklovskii, I. S. , Radioastronomiia . (Radioastronomy.)

Moscow, Gosud. Izdatvo. Tekhniko-Teoreticheskoi Lit. , 1955.

294 p. 128 figs. (incl. photos), foot-refs. DLC (QB574. 545

1955) --This revised and enlarged edition of the 1953 text contains chapters on techniques in radio astronomy, radio radiation from a quiet and from a disturbed sun, from the moon,

from the galaxy, hydrogen (21 cm) radiation, radio stars and

their discovery, cosmic rays and relation to galactic radio

radiation, radio nebulae, radio galaxies and relation to the

metagalaxies, and radiolocation in astronomy. Many illustrations of equipment and results of photography and recording of radiation from galaxies by optical and radio means in

the U. S. S. R. are included for popular, as well as scientific

use (25,000 copies published). Chapters on radio nebulae

and location of discrete sources have been considerably en- larged and brought up to date. (Met. Abst. 11. 6-141. )--M. R.

D-751 Shklovskii, I. S. , Kosmicheskoe radioizluchenie. (Cosmic

radio frequency radiation. ) Moscow, Gosud. Izdatvo. Tekhniko-Teoreticheskoi Lit. , 1956. 492 p. 167 figs. (incl.

photos), 25 tables, 220 refs. , eqs. DLC (QB475. S42) (3000

copies). Transl. into English by Richard B. Rodman and

Carlos M. Varsavsky with title, Cosmic radio waves, issued

Cambridge, Mass. , Harvard Univ. Press, 1960. 444 p. 205

figs. , 27 tables, bibliog. p. 414-428, eqs. DLC--

274
A standard monograph or textbook on radio astronomy for scientists and technicians, covering in 27 chapters (grouped in

6 sections) the following aspects: History of radio astronomy

since JANSKY's discovery 25 yrs ago, antennas and equipment, basic results of observations of cosmic radio radiation,

nature of Galactic radio radiation, monochromatic radiation

from the Galaxy (21 cm), radio astronomy and problems of the

origin of cosmic rays, and finally, radio radiation from the

metagalaxy and its contribution to cosmology. The book emphasizes radiation from outside the solar system. (Met. Abst.

11. 6-140. )-M.R.

D-752 Shklovskii, I. S. (Inst, for Atmos. Physics, Acad, of Sci. of

the U. S. S. R. , Moscow), Elementary processes in the upper

atmosphere and their manifestation in emissions . Annales de

Geophysique, Paris, 14(4):414-424, Oct. /Dec. 1958. 17 refs.,

5 eqs. DLC--This article is subdivided into three chapters,

a) New type of fluorescence in the upper layers of the terrestrial atmosphere; b) Some remarks on the excitation of H

emission in aurorae; c) Interplanetary gas and some geophysical problems. Of the great variety of elementary processes in

the upper atmosphere, leading to the emission of various lines

and bands observed in the spectra of the night airglow and aurorae, only the principal ones are discussed. Among their

number is a new type of fluorescence in the upper atmosphere

and also the problem of interaction of solar corpuscules with

the atoms and molecules of the terrestrial atmosphere. (Met.

Abst. 10. 8-137. )-A.V.

D-753 Shklovskii, I. S. , O vozmozhnom vekovom izmenenii potoka

i intensivnosti radioizlucheniia ot nekotorykh diskretnykh

istochnikov. (Secular variation of the flux and intensity of

radio emission from discrete sources. ) Astronomicheskii

Zhurnal, Moscow, 37(2):256-264, March/April 1960. table,

13 refs. , 16 eqs. Russian and English summaries p. 256.

DLC. Transl. into English in Soviet Astronomy AJ, N. Y. , 4(2):243-24G, Sept. /Oct. 1960. DLC--The dependence of the

flux and brightness on radius is obtained for expanding nebulae — the remnants of supernova outbursts — on the basis of

the synchrotron mechanism of radio emission, and also some

simple theoretical considerations. It is shown that this dependence has the form: F <x u.~ 1$ , I OC 1* where

S , in particular, depends on the exponent of the spectrum

of the source. For different sources, /$ varies within the

limits 3. 2 (Crab Nebula) to 7 (remnants of the outburst of the

1604 supernova). The conclusion is reached that the flux of

radio emission from Cassiopeia A should decrease annually

by about 2%. The present day technique of radio astronomical
observations permits the effect deduced by theory to be detected. The fact that galactic sources have a smaller spectrum exponent than the extragalactic sources is explained.

The intensity of emission from remnants of outbursts at different stages of evolution is considered. At comparatively early

stages, the emission should be exceedingly large. It is concluded that the possibility of observations of radio emission

from supernovae of 1885 and 1895 in M 31 and NGC 5253 is

not excluded. (Met. Abst. 11L-111. )--Author's abstract.

D-754 Shternfel'd, A. A. , Artificial satellites . 2d rev. and extended edition. Moscow, State Publishing House for Technical

and Theoretical Literature, 1958. Transl. of the original Russian (Iskusstvennye Sputniki, pub. 1958) prepared by Technical Documents Liaison Office, Wright -Patters on Air Force

Base, Ohio. Distributed by U. S. Dept of Commerce, Office

of Technical Services, Wash., D. C. 424 p. 58 figs. , 32

plates, 51 tables, 6 refs. Price: $6. 00. DWB (629. 1388

S561isE, 1958). First Russian ed. with title Iskusstvennye

sputniki zemli, issued Moscow, 1S56. Second ed. is greatly

revised owing to launching of 2 Soviet sputniks in Oct. and

Nov. 1957. --Laws of motion, rocket launcher, launching, construction of satellite, human problems, conditions as observed

aboard a satellite, observation and communication from satellite, descent to earth, artificial moon, planet and solar satellites, use of satellites as observatories or stations in space,

interplanetary flight and lav are treated in separate chapters.

Chapter on artificial satellites of other bodies of the solar system is new and accounted for omitting "earth" from title as in

1st edition. The work contains many tables of data and diagrams giving quantitative knowledge of mechanics and theory,

as well as actual data from U. S. and U. S. S. R. sources.

(Met. Abst. 10. 7-19.)-M.R.

D-755 Siglin, Pierce W. and Senn, George, Courier communication

satellite. Institution of Electrical Engineers, Journal, 7(80):

504-508, Aug. 1961. 6 figs. , table. DLC--The Courier communication satellite experiment was undertaken to demonstrate

the feasibility an" operational capabilities of a delayed repeater satellite transmission system and to provide a basis for es- timating the usefulness and capacity of long range multi-station

store and forward message handling capability utilizing a satellite vehicle. This article discusses the exchange of messages

between ground stations through the Courier satellite, gives a typical operating sequence and describes the satellite. --Authors'

abstract.

276
D-756 Simaljak, J. and Milerova, A. , Niektore pozorovania pocas

zatmenia slnka v Bratislave dna 30. iuna 1954. (A few observations during the solar eclipse of June 30f 1954 in Bratislava. ), Meteorologicke Zpravy, Prague, 7(5):132-134, 1954.

4 figs. , photo. Russian and German summaries p. 132. DLC

--Values of total light intensity, yellow, red and ultraviolet

light intensity, temperature, cosmic radiation and radio re- ception during the solar eclipse of June 30, 1954, are graphically presented. All values show a marked decrease during

the eclipse, except tropospheric radio reception which definitely improved, possibly as a result of a decrease in ionization intensity. (Met. Abst. 8. 1-357. )-G.T.

D-757 Simon, Paul, Les eruptions chromospheriques associees aux

sursauts radioelectriques de type IV: effets ionospheriques

et qeomaqnetiques . (The chromospheric flares associated

with the radio-electric outbursts of type IV: ionospheric and

geomagnetic effects. ) Annales d'Astrophysique, Paris, 23(1):

102-110, Jan. /Feb. 1960. 5 figs. , 13 refs. French, English

and Russian summaries. DLC--The chromospheric flares associated with the radio-electric outburst of type IV are intimately

related to the ionospheric disturbances with sudden commencement, the most important of these flares giving rise to particularly severe geomagnetic perturbations. (Met. Abst. unpub.

--Author's abstract.

D-758 Singer, S. F. (Dept. of Physics, Univ. of Maryland), Research in the upper atmosphere with high altitude sounding

rockets. (In: Beer, Arthur, (ed. ), Vistas in astronomy, pub.

London, 1955-1956. Vol. 2:878-912. 23 figs. , 3 tables, bibliog. p. 910-912.) DLC, DWB (520. 82 B415v) -High altitude

rockets have been used to investigate extraterrestrial radiations and the properties of the atmosphere. This article sur- veys the outstanding results achieved in these studies, including: direct measurements of the solar ultraviolet and X radiation; composition and energy spectrum of the primary cosmic

rays; the incidence of micrometeorites; the dependence on altitude up to 220 km of atmospheric pressure, density, temperature, and composition; the distribution of ozone with height;

evidence on the intensity and origin of the day airglow; the

electron and ion density distribution in the ionospheric layers

up to 350 km; variation of the earth's magnetic field with altitude; evidence on the location of ionospheric current sheets

and conclusions about the conductivity of the ionosphere; highaltitude photography and its applications. Characteristics are given of high altitude sounding rockets used in the U. S. : V-2,

Aerobee, Viking and Deacon. Suggestions are made for over- coming some of their inherent limitations to allow expansion of

277
possibilities of high altitude studies. Arguments are presented for the usefulness of instrumented artificial satellite

rockets for astrophysical research. (Met. Abst. 10. 6-91. ) --Author's abstract.

D-759 Singer, S. F. , The artificial earth satellite. Discovery,

17(4): 140-145, April 1956. 7 figs. DLC--A description and

plan of MOUSE are given, with an account of its 90 min orbit

and the path swept out. Knowledge to be gained about radiation and corpuscles outside nearly all the atmosphere is discussed; this will be especially important in study of cosmic

rays. (Met. Abst. 8. 6-64. )--C. E. P. B.

D-760 Singer, S. F. (Univ. of Maryland, College Park), The artifi - cial earth satellite: past, present and future. (1956?) 9 p.

Mimeo. DWB--A brief article outlining the problem of satellite launching and its uses in astronomy, meteorology, (storm

tracking, albedo), study of sun, weather control, etc. , and

details of plans for satellites during IGY. (Met. Abst. 9. 8-

55.)--M.R.

D-761 Singer, S. F. , Satellite instrumentation: results for the IGY.

Franklin Institute, Phila. , Journal. . . Monograph, No. 6:51-70,

Dec. 1958. 12 figs. , 3 refs. DWB (629. 1388 F832te)--The

discussion deals with 1) knowledge gained by the behavior of

uninstrumented satellites; 2) measurements of various kinds

obtainable by satellite-borne instruments; and 3) a comparison

between the Russian and U. S. instrumentation of satellites.

Author's suggestion of a gyroscopic principle for a detector

pointed at the sun or at the earth by means of a spin axis

seems feasible. Likewise the use of solar batteries for storage of information gathered on tapes as a part of the telemetering system which transmits to an earth receiver whenever

a radar beacon hits the receiver. The meteorological gain,

particularly as derived from albedo measurements of the earth

is inestimable. WEXLER's (U. S. Weather Bureau) concept

(depicted here) of the North American continent as seen from

4000 mi altitude is quite illustrative in this respect. The

electrical charge (if any) of a satellite and how it changes is a problem for which instrumentation is considered. (Met.

Abst. 11J-156.)-W. N.

D-762 Sinton, William M. (Johns Hopkins Univ.), Observations of

solar and lunar radiation at 1. 5 millimeters. Optical Society

of America, Journal, 45(ll):975-979, Nov. 1955. 7 figs.

,

table, 7 refs. DWB, DLC- -Observations of the radiation from

the sun and the moon in a wide wavelength band centered approximately at 1. 5 mm are reported. These waves were

278
detected with a Golay detector using a searchlight mirror for a telescope. Measurements of atmospheric extinction are reported and compared with calculations of water vapor absorption which have been made by J.H. VAN VLECK. It is

found that the measured extinction is greater than the calculated. Observations of the radiation emitted by the moon

at different phases are reported. The transmittances of some

materials to the 1. 5 mm waves from the sun are included.

(Met. Abst. 8. 3-182. )--Author's abstract.

D-763 Sisco, W. B. and Fiskin, J. M. , Shock wave ionization and

its effect in space communication. Douglas Aircraft Co. , Long Beach, Paper No. 656, June 1958. (Unchecked).

D-764 Sivaramakrishnan, M.V., Some geomagnetic disturbances

at Alibag Observatory (India) and allied radio and solar effects (1937-1946) . Indian Journal of Meteorology and Geophysics, 1(3):207-219, July 1950. 8 figs. , table, 16 refs.

MH-BH--The phenomena of solar flare and radio fade-out and

the ionospheric disturbances associated with four magnetic

storms recorded at Alibag Obs. are described in detail, and

time of travel of solar corpuscles from sun to earth is considered. A test of intense solar flares with radio fade-out

and sudden pulses in Alibag magnetic traces as counterpart

and the associated magnetic storms the next day for the period 1937-1946 is given. The magnetograms of the individual

magnetic storms are compared, the characteristics of the

magnetic storms are discussed, the causes of the observed

phenomena are indicated and criteria for predicting the oc- currence of great magnetic storms are given. (Met. Abst.

2.2-173.)-I.L.D.

D-765 Skeib, G. , Per Einfluss der Sonnenfinsternis auf die Ausbreitung atmosphcirischer St&rungen im Bereich von 5 kHz bis

30 kHz. (Effect of solar eclipse upon the propagation of atmospheric disturbances in the region of 5 kHz to 30 kHz.)

Germany. Deutsche Demokratische Republik. Meteorologischer und Hydrologischer Dienst, Veroffentlichungen, No.

16:24-27, 1955, 2 figs. DWB, DLC--Effect of eclipse noticed in positive deviation of the number of atmospherics on

30 kHz with a lag of 15 min and a very sharply pronounced

100% deviation in the 5 kHz field strength of atmospherics.

The latter is difficult to explain, since an opposite effect

was expected. No effect was observed in the number of atmospherics on 10 kHz. (Met. Abst. 8. 1-391. )--A. A.

279
D-766 Skilling, William Thompson (San Diego State College, ret'd)

and Richardson, Robert S. (Mt. Wilson and Palomar Obs. ),

Brief text in astronomy. New York, Henry Holt, 1954. 327

p. figs. , tables, photos, charts, bibliog, p. 289-290. DLC

--This elementary but up-to-date text on astronomy contains

many sections which touch on meteorology or climatology.

The atmosphere (composition, refraction, twinkling and geomagnetism) is discussed on p. 34-37; meteorites, zodiacal

light, counterglow on p. 45-50; time and seasons, p. 59-75;

moon's temperature and atmosphere, p. 99-103; eclipses,

p. 113-120; the solar atmosphere, solar and terrestrial relations, radio astronomy, p. 126-153; planetary atmospheres,

albedo, surface temperature, etc ., p. 154-186; and meteors,

p. 197-204. The text is well illustrated and has a good index and glossary of astronomical terms. (Met. Abst. 6. 11-

8.)--M.R.

D-767 Skuridin, G. A. and Kurnosova, L.V., Nauchnye issledovaniia pri pomoshchi iskusstvennykh sputnikov Zemli. (Scientific investigations by means of artificial earth satellites.

)

Priroda, Moscow, 46(12):7-14, Dec. 1957. 6 figs. DLC--

The successful launching on Nov. 3, 1957 of the second

Soviet earth satellite, the information on its movement and

the recordings of instruments mounted in it, make it possible

to obtain very important data on atmospheric conditions at

heights up to 1700 km, to measure the full intensity of cosmic rays at such heights and to register the ultraviolet and

X-radiations of the sun. The authors examine some of the

scientific problems whose solutions seem to have become

possible with the aid of earth satellites. These are investigations of: the short wave portions of the solar spectrum, the

structure of the atmosphere, the corpuscular radiation of the

sun, the solid component of interplanetary substance, and

geomagnetic measurements. (Met. Abst. 10. 4-75. )--A. M. P.

D-768 Slee, O.B. (Div. of Radiophysics, C.S.I. R.O., Univ.

Grounds, Sydney), Apparent intensity variations of the radio

source Hydra -A. Australian Journal of Physics, Melbourne,

8(4):498-507, Dec. 1955. 5 figs. , 2 tables, 7 refs. DLC--

This paper describes the results of a detailed study of the

flux density of the discrete radio source, Hydra-A. Over a period of 12 months, approximately 200 measurements of the

Hydra-A intensity was compared with a similar number of observations on other strong sources. It was concluded that

the observed flux density of Hydra-A is much more variable

than that of these other sources, although no periodic

changes have yet been detected. Possible mechanisms for

the observed intensity changes are discussed. (Met. Abst.

9A-93.) --Author's abstract.

280
D-769 Slonim, Iu. M. , Moshchnye khromosfernye vspyshki 10 i 14 iiulia 1959 q. (Intense chromospheric flares of July 10

and 14, 1959.) Astronomicheskii Zhurnal, Moscow, 37(2):

347-349, March/April 1960. 2 figs. , table, ref. Russian

and English summaries p. 347-348. Transl. into English in

Soviet Astronomy AJ, N.Y. , 4(2):327-330, 1960. DLC--

Results are given of observations of two intense chromospheric flares, which appeared on July 10 and^ 14 above a

large, irregular sunspot. A similarity in the structure of

the flares is noted. Their development is evidence of eddy,

or pseudoeddy, motions and of a systematic movement of

the principal emission node in a western direction. The

ionospheric effects due to these flares are described. (Met.

Abst. 11L-269.) -Author's abstract.

D-770 Smith, Alex G. ; Carr, T. D. and Perkins, W. H. (all, Florida

Univ. , Gainesville), Anomalous night-time reception of a major solar radio burst. Nature, London, 183(4661):597-598,

Feb. 28, 1959. fig. , 3 refs. DWB--The University of Florida

Radio Observatory had Jupiter under observation on five different receiving arrays the morning hours of March 8, 1958,

when at 0235 U. T. a single very intense burst of noise rising

slowly and decreasing more slowly over a 2 min period was

simultaneously observed on all five channels. Characteristics of a solar burst rather than a Jupiter pulse were identified at sunlit observation sites elsewhere. Hence, the major

solar burst was propagated somehow far into the earth's dark

hemisphere. Position of the celestial bodies concerned is

shown in a diagram. (Met. Abst. 11. 8-78. )--W. N.

D-771 Smith, A. G. , Extraterrestrial noise as a factor in space communications. Institute of Radio Engineers, N. Y. , Proceedings, 48(4): 593-599, April 1960. 4 figs. , 2 tables, 22 refs.

DLC--Present-day refinements in communication systems make

it appear that extraterrestrial noise sources may establish a fundamental limitation on long-range communications. The

various cosmic and solar system radio sources are considered with respect to their intensities, spectral distributions,

and temporal characteristics. The most severe forms of interference occur in the long wave length regions of the radio

frequency spectrum, so that the future of space communications probably lies in the perfecting of low-noise microwave

systems. (Met. Abst. 11. 10-50. ) --Author's abstract.

D-772 Smith, A. G. ; Carr, T. D. ; Bollhagen, H. ; Chatterton, N.

and Six, F. , Ionospheric modification of the radio emission

from Jupiter. Nature, London, 187(4737): 568-570, Aug. 13,

1960. DLC--

281
The experiment of Gardner and Shain has been repeated at

18 Mc using two identical receivers separated by 7040 km.

Some correlation is found between records at the two sites

but there is also evidence of serious distortion caused by

terrestrial effects. --IRE Abst. 3472

D-773 Smith, F.Graham; Little, C. G. and Lovell, A. C.B. , Origin

of the fluctuations in the intensity of radio waves from galac - tic sources. Nature, London, 165(4194) :422-425, March 18,

1950. 6 figs. , 2 tables, 8 refs. DLC--Smith reports on the

experimental observations at Cambridge using 6. 7 m wavelength receivers spaced up to 170 km. Two types of fluctuations indicate two separate mechanisms; one related to var- iation of emission from sources, the other to diffraction in a more or less local region. Little and Lovell report on measurements of radiation from Cygnus and Cassiopeia as conducted between May 1 and Oct. 31, 1949, in cooperation

with Smith, using 3. 7 m wavelength at both Jodrell Bank and

Cambridge, 210 km distant. Results show radiation to be

either steady at both sites, or fluctuating at both sites, on

a given night. No correlation between disturbances when

fluctuations occurred at both sites, and if on one side only,

the significant exceptions were about 10%. --W. N.

D-774 Smith, F. G. , Ionospheric refraction of 81. 5 Mc/s radio

waves from radio stars. Journal of Atmospheric and Terrestrial Physics, 2(6):350-355, 1952. 3 figs., 8 refs. DWB--

Apparent regular movements of 4 radio stars are ascribed to

"wedge refraction/' i. e. , to E-W gradients of the total electron content of the ionosphere. (Met. Abst. 4.6-90.)--

C. E. P. B.

D-775 Smith, F. G. (Mullard Radio Astron. Obs. , Univ. of Cambridge), The possibility of observing features of galactic

radio emission from a satellite-borne radio telescope. Royal

Astronomical Society, London, Monthly Notices, 122(6):527-

534, 1961. 6 figs. , 6 refs. , eqs. DLC--It has already been

proposed to extend measurements of the spectrum of radio

emission from the galaxy to frequencies of about 1 Mc/s by

means of a satellite-borne receiver. If the satellite is in

the upper ionosphere, where the refractive index is increasing with height, a focusing effect will occur which may allow individual features of emission to be observed. It is

shown that a beamwidth of the order of 20 may be achieved

under favorable circumstances; the most important limitation

is the frequency bandwidth necessary in a sufficiently sensitive receiver, which inevitably means that dispersion in the

282
refractive index effectively blurs out any narrower beam or any interference effects inside the beam. The experimental

conditions needed for the realization of this degree of focusing in a satellite or a rocket flight are discussed. It appears that the frequency of a satellite-borne receiver should

sweep over a range of about 3 to 5 Mc/s, with a bandwidth

of 10 kc/s. The satellite orbit should be nearly circular, at a height of about 400-500 km. (Met. Abst. unpub. ) -Author's abstract.

D-776 Smith, Harlan J. and Douglas, J. N. (both, Yale Univ. , New

Haven), Observations of planetary nonthermal radiation.

(In: Paris Symposium on Radio Astronomy, July-Aug. 1958,

(Proceedings), pub. Stanford Univ. Press, 1959. p. 53-55.

3 figs. , ref.) DLC (QB475.P26) -Observations of Jupiter

and Saturn at 23. Mc/s were made and are analyzed. Results indicate that Saturn is a doubtful though possible

source of radiation; that Jupiter in the last two years has

shown burst occurrence probabilities roughly in the ratio

1:0.8-0. 1 for frequencies 18, 21 and 23 Mc/s; and that

there is good correlation between the longer pulse elements

of storms over 0. 8 Mc/s frequency separation around 23

Mc/s and between sites separated by tens of miles.—A. J. M.

and authors' conclusions.

D-777 Smith, R.L. and Helliwell, R.A. (both, Stanford Univ. ),

Electron densities to 5 earth radii deduced from nose whistlers. (Summary only. ) Journal of Geophysical Research,

Wash., D.C., 65(9):2583, Sept. 1960. fig. DLC-Whistlers appear to propagate in columns of enhanced ionization

aligned with the earth's magnetic field. From nose whistlers a value of 100 electrons/cm^ is calculated at 5 earth

radii. (Met. Abst. 11. 12-328. ) -Authors' abstract.

D-778 Smith, R.L. ; Helliwell, R.A. and Yabroff, I. W. , A theory

of trapping of whistlers in field aligned columns of enhanced

ionization. Journal of Geophysical Research, Wash. , D. C,

65(3):815-823, March 1960. 8 figs. , table, 15 refs. , 11

eqs. DLC--A ray theory of whistler propagation in ducts is

developed for the purpose of explaining discrete whistler

components. By use of refractive index surfaces and a Snell's law construction, it is shown that the only feature

of the electron distribution affecting the trapping conditions

is the ratio of the electron density in the column to that of

the background. In most practical cases the electron density in the column required for trapping must be greater than

the background level. Under certain conditions, however,

the density in the column must be less than the background

283
level. Using the theory/ it is found that the enhancement

required for trapping increases markedly toward the equator,

providing a possible explanation for reduced whistler occur- rence at the lower latitudes. (Met. Abst. 11. 12-326.)--

Authors" abstract.

D-779 Smith-Rose, R.L. , International research in radio astronomy. Nature, London, 176(4493): 1110-1111, Dec. 10, 1955.

3 refs. DWB--Summary of special reports 3-5 of the International Scientific Radio Union: 3) Discrete sources of extraterrestrial radio noise; 4) Distribution of brightness on the

solar disk; 5) Interstellar hydrogen. (Met. Abst. 8. 1-112. ) --C. E. P. B.

D-780 Sirensen, E. V. , Magneto-ionic Faraday rotation of the

radio signals on 40 Mc/s from Satellite 1957 (Sputnik I).

(Abstract of article issued by Danish Academy of Technical

Sciences, Microwave Laboratory, Copenhagen, as its Report P 1765, June 24, 1959). -Some of the fadings of the 40

Mc/s signals from Sputnik I during morning transits are as- sumed to originate in Faraday rotation in the ionosphere.

This has been investigated for the transit of Oct. 12, 1957,

5. 30 GMT, for which the orbit was known with reasonable

accuracy. The fading records show an increasing fading

rate during the last part of the transit. This is contrary to

the simple theory based on the assumptions of a flat earth

and a homogeneous ionosphere, from which a constant fading rate should be expected. The main reason why simple

theory did not apply in this case, is that the satellite travels through the twilight zone from night towards day, i. e.

,

from low to high ionization. The Faraday rotation is calculated by means of data for the orbit, magnetic field maps

and predictions of the ionosphere conditions. The result

is in good agreement with the observation when a high ionization between the altitude of maximum ionization and the

satellite is assumed. The effect of refraction is estimated

by means of the perturbation theory. It increases the Faraday rotation from to 19% during the transit. It is concluded that it is difficult to obtain detailed information on the

state of the ionosphere by means of such fading records,

especially when the frequency is so low that the refraction

becomes significant. (Met. Abst. 11F-140. ) --Author's

abstract.

D-781 Soifer, Raphael (M. I. T. , Cambridge, Mass. ), Satellite

supported communication at 21 megacycles. Institute of

Radio Engineers, N. Y. , Proceedings, 49(9): 1455-1456,

Sept. 1961. table, 3 refs. DLC--

284
Coordinated control experiments (Nov. 1959) with WWV signals, were conducted by a group of advanced radio amateurs

over the path New York, N. Y. and Bethesda, Md. The tests

were conducted when the ionosphere did not support normal

communication, hence, no audible background levels, and

when satellites were expected an,d not. Tabulated three interval scheme results of burst frequency are discussed briefly. The main object was to achieve a two way communication which was met with success. Improvement of range and

effectiveness are in process. --W. N.' D-782 Solar eclipses and the ionosphere: a symposium held under

the auspices of the International Council of Scientific Unions

Mixed Commission on the Ionosphere, in London, Aug. 1955. Editors, W. J. G.Beynon and G. M. Brown, London, Pergamon,

1956. 330 p. figs. , tables, eqs. refs. at end of each ch.

Literature on solar eclipses and the ionosphere (including)

chronological catalogue of eclipses, p. 308-320 (225 refs.).

Issued as Vol. 6 of the Special Supplements to the Journal of

Atmospheric and Terrestrial Physics. DWB. Review by R.

M. Goody in Weather, 12(6):198, June 1957. Review by R.

L. Smith-Rose in Mature, London, 179(4562) :711, April 6,

1957. Also: Beynon, W. J. G. , Solar eclipses and the ionosphere. Nature, London, 176(4490) .-947-948, Nov. 1955.

D-783 Somayajulu, Y. V. and Narayana Rao, N. (both, Madras

Inst, of Technology, Chromepet, Madras), Observations on

galactic radiation at 30 Mc/s. Journal of Scientific and Industrial Research, Sec. A, New Delhi, 17(12); Special Supplement, Dec. 1958. p. 54-56. 2 figs. , 8 refs. DWB, DLC

--A Philips BX 925 A receiver, bandwidth 2. 6 kc/s was used

in the observations outside Madras since Oct. 1957, discussed briefly accompanied by plot of diurnal variation of

the cosmic noise intensity, which rapidly increases after

sunset, decreases after sunrise. (Met. Abst. 12. 1-134.

)

-W. N.

D-784 Southworth, George C. (Bell Telephone Labs. ), Early history of radio astronomy. Scientific Monthly, Wash., D. C.

,

82(2):55-67, Feb. 1956. 12 figs. (incl. photos), 10 refs.

and notes. DWB, DLC --The author relates the history of the

discovery of radio waves from the Milky Way by JANSKY in

1931 and of radio waves from the sun in 1942 by the author

and other investigators. The historical account is based in

part upon the author's memory of events in which he participated personally, and upon the notes of various investigators.

The existing knowledge of the radio spectrum, the work on

long wave static measurements carried out in the Bell Telephone Laboratories by FRIES, the beginning of short wave

285

^*
static measurements by JANSKY (diagrams of the circuit used

by JANSKY during his discovery of radio waves from the Milky

Way is shown), the steps toward the discovery of radio waves

emanating from the Milky Way, and GROTE REBER's studies

of extraterrestrial noise, and SOUTHWORTH's own work leading to the discovery of radio waves from the sun are reviewed.

Photographs of apparatus used, samples of records obtained

are presented. (Met. Abst. 9A-134. )--I. L. D.

D-785 Spitz, Armand and Gaynor, Frank, Dictionary of astronomy

and astronautics. N. Y. , Philosophical Library, 1959. 439 p.

--Short, terse definitions of over 2000 terms in astronomy,

astronautics and upper atmospheric physics, are included in

this up-to-date glossary. Some of the terms are defined at

greater length and a great deal of astronomical data about

the sun, moon, planets and their orbits and satellites, constellations plus some excellent photographs of the moon,

Saturn, sunspots, etc. , are included. Most of the constellations, recent artificial satellite programs, and some astrological terms are defined. (Met. Abst. 10. 8-78. )--M. R.

D-786 Sprenger. K. and Lauter, E. A. , Beobachtungen der tiefen

Ionosphare walhrend der Sonnenfinsternis am 30. 6. 1954, (Observations of the low ionosphere during the solar eclipse

of June 30, 1954.) Beitra'ge zur Geophysik, Stuttgart, 64(4):

284-312, 1955. 17 figs. , 14 refs. DWB-At Kuhlingsbom

on 185-1223 kHz the expected increase of the reflection coefficient of the low ionosphere did not appear until some time

after the first contact, and normal values returned considerably before the end of the eclipse. The observed effect (40

db) and retardation of the maximum (4 min) agreed with calculation from a single layer model of the D region, but the

time contraction is only reconciliable with a multiple structure. Observations of the level of disturbance in the long

wave region (8-70 kHz) show first a positive phase due to a decrease of low ionosphere damping, followed by a long

negative phase after the maximum obscuration, apparently

due to meteorological effects of the eclipse. (Met. Abst.

7. 1-189.)-C.E.P.B.

D-787 Stanley, G. J. and Price, R. , An investigation of monochromatic radio emission of deuterium from the galaxy. Nature,

London, 177(4522): 1221-1222, June 30, 1956. 3 figs. , 4 refs.

DWB--Observations at Sydney, Australia, of radiation from

the center of the galaxy on a frequency of 327. 555-327. 369

Mc/s showed that temperature of critical source is 800 K and

abundance of deuterium is less than 10"3 that of hydrogen.

(Met. Abst. 9A-135. )--C.E.P.B.

286
D-788 Staras, H. (RCA Labs. , Princeton, N. J. ), The propagation of wide band signals through the ionosphere. Institute

of Radio Engineers, N. Y. , Proceedings, 49(7):1211, July

1961. 2 refs. , 7 eqs. DLC--The differential group delay

across the frequency band is discussed in relation to wide

band satellite techniques. The estimated delays given are

restricted to a reasonably regular ionosphere (no flare distuptions). Quantitative values depend on satellite tests

designed for this purpose. (Met. Abst. unpub. )--W. N.

D-789 Sternberg, Sidney (RCA Astro-Electronic Products Div. , Princeton, N. J.) and Stroud, William G. (NASA Goidard

Space Flight Center, Beltsville, Md. ), Tiros I: meteorological satellite . Astronautics, N. Y. , 5(6):32-34, 84-86,

June 1960. figs. , photos. DLC--The first two weeks operation of Tiros I proved the feasibility of using television camera equipped satellites for viewing the earth cloud cover and

returning pictures of large clouded areas back to earth. Some

of the representative cloud pictures, the launching of the

weather satellite, a cutaway view of major components and

the relative camera coverage areas are shown. The Tiros I exceeded expectations and its success predicts a brilliant

future for such observation satellites and world-wide meteorology. (Met. Abst. 11J-166. )--E. K.

D-790 Stetson, Harlan T. , The sun and the atmosphere . Smithsonian Institution, Annual Report, 1938:149-174. 7 figs. , 3 plates. DLC--A popular account of radiations from the

sun and their effects on the earth's atmosphere, frequency

of auroras, geomagnetism, radio reception, temperatures

and weather, especially relations to the sunspot cycle. The

theory of sunspots is discussed. (Met. Abst. 8A-20. ) D-791 Stoffregen, W. (Ionosphere Observatory, Upsala), Solar

eclipse of June 30, 1954: preliminary report. (In: Solar

eclipses and the ionosphere: a symposium. . . ed. by W. J. G.

Beynon and G. M. Brown. London, Pergamon, 1956. p. 57-

64. 11 figs. , 2 tables). DWB--Ionospheric measurements

at two stations in Sweden during the eclipse of June 30, 1954

are summarized. The behavior of the Es layer was similar to

that of the E and F layers during the eclipse, but some hours

before the eclipse the Es ionization was high. Field strength

measurements for long and medium waves indicated a short,

sharp increase near the eclipse maximum. The noise level of

atmospherics was also greater during eclipse. (Met. Abst.

9. 6-267. ) -Author's abstract.

287
D-792 Storey, L. R.O. , A method to detect the presence of ionized hydrogen in the outer atmosphere . Canadian Journal of

Physics, 34(11): 1153-1163, Nov. 1956. 4 figs. , table, 12

refs. , eqs. DWB, DLC--The method proposed for the detection of ionized hydrogen in the outer atmosphere relies on

the influence of the positive ions on the propagation of whistlers. If ionized hydrogen is the chief constituent of the atmosphere at great heights above the earth, then the relation

between frequency and time in a whistler should depart at

low audio frequencies from the form observed at higher frequencies. The departure is likely to be most marked in

whistlers occurring at low magnetic latitudes. At magnetic

latitude 45 the effect of the hydrogen ions should be detectable at frequencies below about 2 kc/sec. (Met. Abst. 8. 6-

189. )- -Author's abstract.

D-793 Storey, L. R.O. , A method for interpreting the dispersion

curves of whistlers. Canadian Journal of Physics, Ottawa,

35(9): 1107-1122, Sept. 1957. 5 figs. , table, 10 refs. , 30

eqs. DWB, DLC--This paper considers how the dispersion

curves of whistlers may be interpreted to provide information

on the distribution of electron density with height in the outer atmosphere. The simpler inverse problem, that of computing the dispersion curve for a given distribution, is considered first. On the assumption of longitudinal propagation in a dipole magnetic field, the dispersion curve is derived in

the form of an equation relating the product tf^ to the frequency f. The equation can be represented by a power ser- ies in f , which is useful for estimating departures from the

elementary f - & - t relationship at frequencies where these

departures are small. The coefficient of f in this series is

termed the "dispersion constant of order n" The main problem is now treated, regarding the above equation as an integral equation determining the distribution of electron density

along the path. This integral equation is solved in series,

making use of the same power series in f . The dispersion

constant of order n is shown to be proportional to the nth

moment of the distribution, suitably expressed and weighed.

From the values of the moments, it is possible to deduce

both the initial geomagnetic latitude of the path and the distribution of electron density along it. When the observed

dispersion curve is incomplete, so that only the dispersion

constants of lower order can be measured, the method yields

an approximation to the distribution. (Met. Abst. 9. 7-279. ) --Author's abstract.

288
D-794 Storey, L. R.O. , A method for measuring local electron density from an artificial satellite. U. S. National Bureau of

Standards, Journal of Research, Sec. D, 63(3): 325-340, Nov./

Dec. 1959. 11 figs. , table, 14 refs. , 51 eqs. DWB, DLC--

A method is proposed for measuring the electron density at

known points in the outer ionosphere, by the use of VLF re- ceiving equipment in an artificial satellite, in conjunction

with a VLF transmitter on the ground. The transmitter would

radiate continuous waves, which would be propagated through

the ionosphere in the "whistler" mode. The basis of the method is a measurement of the local wave admittance of the medium, by comparison of the signals received on an electric dipole and on a loop. A further proposal is made for an integrated VLF satellite experiment, in which several different

types of observations would be made simultaneously. (Met.

Abst. 11F-141.) -Author's abstract.

D-795 Storey, Owen (Defence Res. Board, Ottawa), Protons outside the earth's atmosphere. Annales de Geophysique, Paris,

14(2): 144-153, April/June 1958. 4 figs., 6 refs., 4 eqs.

French and English summaries p. 144. DLC--The evidence

is surveyed for the belief that hydrogen is the main ionizing

constituent of the earth's atmosphere at great heights. If

this view is correct, it should be possible to detect the protons by making precise measurements of the dispersion curves

of whistling atmospherics observed at low latitudes. (Met.

Abst. 10. 2-155. ) -Author's abstract.

D-796 Stranz, Dietrich, Ergebnis einer Fade-out-Statistik. (Results of fade out statistics. ) Archiv der elektrischen Ubertragung, 4:217-218, (1950). 7 refs. Reprint available.

MH-BH--Distribution of spots about central meridian of sun

on days with total fading and without fading at GSteborg compared for Aug. -Dec. 1948. This showed a significant rarity

of spots near central meridian on days without fading. (Met.

Abst. 2.8-173.)--C.E.P.B.

D-797 Stratton, F. J. M. (Caius College, Cambridge), Radio astron - omy. Pakistan Journal of Science, Lahore, 6(3): 137-141, July

1954. DWB--The science of radio astronomy was born on Feb.

26, 1942, in England when all radar sets reported unidentified

noise, later found to come from the sun. The science could

not be developed until after the war when radar sets became

surplus and were used for nonmilitary research such as detecting meteors or charged particles in the train of a meteor.

Also, disturbances on the sun or in the chromosphere can be

mapped; eclipses do not completely block radiations; structure of Milky Way can be determined. Radio stars were first

289
detected in 1932 by JANSKY; now it is found they are not

points (stars) but areas (discrete sources). By observing

radio stars from 3 points the structure or disturbances in

ionosphere can be determined. New 250 ft radio telescope

at Manchester, England, will enable us to see farther into

space than ever before. Finally, hydrogen line (21 cm) is

visible. (Met. Abst. 9A-66. )--M. R.

D-798 Strong, C.L., How a group of amateurs detected flares on

the sun with long wave radio receivers. Scientific American,

N.Y., 203(3): 231 -244, Sept. 1960. 8 figs. DWB, DLC--

David Warshaw of Brooklyn, N. Y. , designed an inexpensive

radio receiver expressly for the purpose of monitoring flare

activity. Despite several delays the first SEA appeared on

his record on Oct. 4. Walter A. Feibelman of Pittsburgh,

Pa. , built a station after Warshaw 's design, and Val Isham

of Powell, Ohio, assisted by G.H. Pieterson, also put a station into operation. The records submitted by these stations

compared favorably with those of professional observatories.

Thereafter the Bureau of Standards assigned four Brown re- corders to the project for a peri&d of a year. Additional observers included Ralph Buckstaff, Walter Scott, Franklin

Loehde of Alberta, and Robert Evans of Victoria, B. C. and

C.H.Hossfield of New Jersey. Subsequently a number of

others joined the group. An explanation is given of what is

shown by the SEA recordings. A detailed sunrise pattern

was distinguished. This correlated satisfactorily with those

made by the official observatories and they obtain some

SEA's that are missed by the official stations, and vice

versa. Walter Orr Roberts of the Bureau of Standards noted

that this program is making an important contribution to the

observing effort. (Met. Abst. unpub. )--E. S.

D-799 Stroud, W. G. and Nordberg, W. (Signal Corps. Eng. Labs.

,

Ft. Monmouth, N. J.), Meteorological measurements from a

satellite vehicle. (In: Van Allen, James A. (ed. ), Scientific uses of earth satellites. Ann Arbor, Univ. of Michigan

Press, 1956. p. 119-132. 9 figs. , 3 tables, 12 refs. ) DWB

--Among the meteorological observations which could be made

from an earth satellite are albedo measurements with a photodetector. The satellite must be capable of giving orientation

information. The theory, variations with latitude, time of

day and season, and for various types of surfaces (snow, rock,

vegetation, sea, clouds), for various wavelengths, cloud

thickness, etc., methods and instruments, orientation and

telemetering problems and operational requirements are discussed and illustrated with graphs, charts and diagrams.

(Met. Abst. 11J-168.)--M.R.

290
D-800 Struve, O. ; Emberson, R. M. and Findlay, J. W. (all, Nat'l.

Radio Astronomy Obs. , Green Bank, W. Virginia), The 140

ft radio telescope of the National Radio Astronomy Observa- tory. Astronomical Society of the Pacific, San Francisco,

Publications, 72(429) :439-458, Dec. 1960. fig. , foot-ref.

DLC--The 140 ft telescope is intended to be of the family of

precision instruments in the U. S. It will be used as a re- search tool for measuring accurate positions of small radio

sources and maps of larger sources, for determining radiative fluxes of many sources at different frequencies, for

studying variable sources, as well as refraction and scintillation of radiowaves. The performance specifications of the

telescope require operation at wavelengths at least of 3 cm

and suitability for photometric and positional program. The

operation of drive and control should be consistent with the

required accuracy. The above performance requirements

were translated into structural and mechanical specifications, described in detail. Dimensions of the telescope

are presented in a table. (Met. Abst. unpub. )--S. N.

D-801 Suzuki, Shigemasa (Tokyo Astron. Obs. ), Multiphase radio

interferometers for locating the sources of the solar radio

emission. Astronomical Society of Japan, Tokyo, Publications, 11(4): 195-215, 1959. 16 figs. , 8 refs. , numerous

eqs. DLC- -Multiphase radio interferometers, developed for

the purpose of minimizing the ambiguity and simplifying the

reduction procedure in locating the sources of the solar ra- dio emission, are discussed. By simple eye estimation, the

relative position can be deduced with an accuracy of 0. 01 R.

(Met. Abst. 11L-83. )--Author's abstract.

D-802 Svensson, S. I. ; Hellgren, G. and Perers, O. , The Swedish

Radioscientific Solar Eclipse Expedition to Italy, 1952: preliminary report. Goteborg, Sweden. Chalmers Tekniska Hogskola, Handlingar, No. 181(its subseries Electrical Engineering Series, Vol. 7, No. 6), 1956. 30 p. 20 figs. , 15 refs.,

eq. DWB, DLC. Also issued as: Acta Polytechnica, Stockholm, No. 212, 1957. --Pt. I of the report accounts for the

ionospheric part of the expedition. It gives general information of the sweep-recording equipment. Further, it presents

the E, Fl and F2 observations made. The experimental reduction in critical frequency is found to be greater than theoretically predicted. The discrepancy is discussed. Pt. II ac- counts for the solar noise measurements on 2 m wavelength.

General information about equipment and antenna system is

given. Total intensity and the amount of circular polarization of the solar radiation were measured. A short discussion of the observational results is given. (Met. Abst.

11. 7-127. )--Authors" abstract.

291
D-803 Swamp, G. (Stanford Univ. , Calif. ); Stone, P. H. and

Maxwell, Alan (both, Harvard College Obs. , Ft. Davis,

Texas), The association of solar radio bursts with flares

and prominences. Astrophysical Journal, Chicago, 131(3):

725-738, May 1960. 7 figs. , 4 tables, 26 refs. DWB, DLC

--Solar radio bursts in the frequency range 100-580 Mc/s

have been correlated with solar optical phenomena over a 2 yr period covering the present sunspot maximum. It is

found that 60% of fast drift (Type III) radio bursts are coincident in time with solar flares. This figure is in accord

with that obtained by previous investigators, but statistical

studies show that only half this number of bursts are truly

associated with flares; the remainder are associated by

chance. The truly associated bursts usually occur between

the start and the maximum of a flare. Intense bursts are more highly associated with flares than are weak bursts. In

the reverse correlation — that of flares with radio bursts —

it is found that 25% of all solar flares are apparently associated with fast drift bursts, the probability of association

increasing if the flare is of greater area or height, on the

east side of the disk, or accompanied by a surge or spray.

Almost all slow drift bursts (Type II) and continuum (Type

IV) events are associated with flares, often of large area

and intensity, but there is no well defined association between noise storm bursts (Type I) and flares. Only a small

proportion of ejective solar prominences are accompanied by

radio bursts; this may result from the unfavorable geometry

for radio propagation from the limb. Concerning the physical association of the flares and solar bursts, it is suggested that both phenomena result from an unidentified primary

origin. The transfer of energy to coronal radio levels probably takes place at 10^ km/sec in the case of the fastdrift bursts and at about 10^ km/sec for the slow drift bursts.

(Met. Abst. 1 1L -94. )--Authors' abstract.

D-804 Swerling, P. and Crain, C. M. , A possible transponding

system for an artificial asteroid. Rand Corporation, Santa

Monica, Calif. , Project Rand Research Memorandum, RM2172, May 14, 1958. 35 p. figs. , 3 tables, 5 refs. , 34

eqs. DWB (507. 2 R186r)--The measurement of transmission

path length to an artificial asteroid by radio frequency transponding techniques has been suggested as a means of increasing the precision with which the dimensions of the solar system are known. This report describes the design of a possible pulsed transponding system by which the transmission path length could be measured with an accuracy

limited essentially by the accuracy with which the velocity

of light is known, i. e. about one part in 10". Typical

292
values of range and radial velocity with respect to the earth

of the proposed artificial asteroid are assumed. All assumed

components are presently available. A weight and volume

breakdown of a possible design is given, which indicates

that the necessary asteroid-borne transponding equipment,

with associated power sources, could be accommodated in a 15 lb package occupying about 900 cu in. (Met. Abst.

12.4-63. ) --Authors' abstract.

D-805 Swerling, P. , First order error propagation in a staqewise

smoothing procedure for satellite observations. Journal of

the Astronautical Sciences, N. Y. , 6(3):46-52, Autumn

1959. 72 eqs. DWB--A practical method of smoothing satellite data by evaluating a finite number of parameters, or elements, is presented. (Met. Abst. 11. 12-569. )--Author's

abstract.

D-806 Symposium on Ballistic Missiles and Space Technology,

4th. 1959. Proceedings of the 4th AFBMD/STL Symposium

(on) Advances (in) Ballistic Missile and Space Technology.

Co-sponsors, Air Force Ballistic Missile Div. and the Space

Technology Laboratories, Inc. (Proceedings issued in) Planetary and Space Science, N. Y. , Vol. 7, July 1961. 462 p.

figs. , photos, tables, refs.--The entire volume, which is devoted to the proceedings of the symposium, contains 45 papers listed under the following subject headings: Instrumentation and control (4 papers); Space guidance (8); Trajectories (7); Computers (2); Reliability (4); Space communication (3); Man in space (10); Space experiments (7). Abstract of all papers will appear in Meteorological and Geoastrophysical Abstracts; some within the scope of the present bibliography are included here. --W. N.

D-807 Symposium on Physical Processes in the Sun-Earth Environment. July 20-21. 1959. Proceedings. Comp. by C.Collins.

Canada. Defence Research Telecommunications Establishment, Publication No. 1025, March 1960. 392 p. figs.

,

tables, refs. , eqs. DLC--Contains a total of 33 papers; 9

on sun-earth atmospheres, 10 on geomagnetically trapped

particles, 7 on wave interaction and 7 on auroral and magnetic disturbances. Abstracts of all papers will appear in

Meteorological and Geoastrophysical Abstracts. --W. N.

D-808 Symposium on the Plasma Sheath: Its effects on communication and detection, Dec. 1959, Boston, Mass. Electromagnetic effects of re-entry: selected papers from the Symposium.

Ed. by Walter Rotman and Gerald Meltz. Pub. in Planetary

and Space Science, N. Y.,Vol. 6, 1961. 226 p. figs. , tables,

refs. , eqs. "Symposium under auspices of the Electromagnetic

293
Radiation Lab. of the U. S. Air Force Cambridge Research

Lab." The Volume is divided into 4 major sections: A.

Thermodynamic and electrical properties of stock-ionized

flow fields (7 papers). B. Interaction of microwaves and

ionized air (5 papers). C. Voltage breakdown of antennas

(3 papers). D. Experimental techniques for exploring the

interaction of microwave energy with ionized flow field

(5 papers). The term plasma sheath, in contrast to Langmuir's original meaning, is here used to define the envelope of ionized gas produced about a body entering the

atmosphere from outside at hypersonic velocities. Some

of the papers dealing with propagation of radio waves in

the presence of the plasma sheath and its consequent

wake are included in the present bibliography. All abstracts will be published in Meteorological and Geoastrophysical Abstracts. --W. N.

D-809 Syrovatskii, S.I. (Acad. Sci. , U.S.S. R.) f The distribution of relativistic electrons in the galaxy and the spectrum

of synchrotron radio emission. Soviet Astronomy AJf N. Y.,

. 3(l):22-38, Jan. /Feb. 1959. 2 figs. , 10 refs. , 91 eqs.

DLC. Transl. of Raspredelenie reliativistskikh elektronov

v Galaktike i spektr magnitotormoznogo radioizlucheniia,

Astronomicheskii Zhumal, Moscow, 36(l):17-32, Jan. /Feb.

1959. DLC --The problem of the diffusion of particles is

solved, taking into account the regular changes of the particle energy during this process. The spatial distribution

and the energy spectrum of electrons, whose energy changes

because of radiation emission in the magnetic field, was

found on the assumption that the sources occupy an ellipsoidal volume and inject into interstellar space relativistic

electrons with an energy spectrum Q E~ ~Y °. The case when

the distribution of the sources coincides with the flat subsystem of the galaxy and 70= 2 is considered in detail.

The energy spectra of electrons along the line of sight in

different directions and the corresponding intensities of

synchrotron radiation were calculated. It is shown that the

energy spectrum of electrons along the line of sight can be

represented in a limited energy region by the expression

KE y , where "Y varies within the limits 2 <C"y <^3, depending on the choice of the diffusion coefficient. The

choice of the diffusion coefficient of relativistic particles

29

in interstellar space equal to D = 10 cm/sec and the intensity of the sources (the coefficient in the source spec38

trum) Q - 10 ergs/sec give agreement between the theoretical and observed spectra of nonthermal radio emission

of the galaxy in the frequency region JA /» 10 Mc. (Met.

Abst. 11L-106. )--Author's abstract.

294
D-810 Takakura, Tatsuo (Univ. of Tokyo), Polarized bursts and

noise storms of solar radio emission, Pt. 2, Storm bursts

and background continuum. Astronomical Society of Japan,

Tokyo, Publications, ll(2):55-70, 1959. 7 figs. , table,

4 refs. , 53 eqs. Pt. 3, The post-detection low frequency

spectra of noise storms. Ibid. , p. 71-78. 8 figs. , 2 refs.,

8 eqs. DLC--An attempt is made to explain the so-called

background continuum of the noise storms as the superposition of many spikes which have an identical shape, occur

at random and whose amplitudes are distributed according

to a probability density. If two parameters, the frequency

of occurrences of bursts and the range of distribution of

the amplitude, change with time as they are likely to do,

almost all noise storms are in fairly good agreement with

the present hypothesis. In this case, so-called "storm

bursts " are fluctuations about a mean level and the superposition of at least a few spikes. (Met. Abst. 11L-96.

—Author's abstract.

D-811 Takakura, T. (Tokyo Astron. Obs.), Microwave bursts of

solar radio emission. Astronomical Society of Japan, Tokyo,

Publications, 12(l):55-62, 1960. 5 figs. , 3 refs. DLC--

Wide-band compound dynamic spectra of solar radio outbursts have been studied in the frequency range from 9500

Mc to 67 Mc. The range of 9500-1000 Mc has been covered

by the records at several fixed frequencies, and both the

swept frequency records and fixed frequency records have

been used on the frequencies below 1000 Mc. A typical

outstanding outburst may be as follows. A short lived

burst whose duration is several minutes begins almost simultaneously at the frequencies above 1000 Mc. The flux

density of the burst is maximum at about 9000 Mc - 3000

Mc, decreases with decreasing frequency and is generally

very weak on the frequencies below 1000 Mc. A few minutes later, a Type II burst begins in the meter wave region

with a sharp high frequency cut-off which is usually below

350 Mc for the fundamental wave (and below 700 Mc for the

second harmonic). Following the Type II burst, a broadband Type IV burst begins and lasts one hour or two. The

frequencies for the maximum flux density of the Type IV

bursts distribute depending on the case from 200 Mc to

10, 000 Mc. Above mentioned short lived burst at the frequencies above 1000 Mc is neither an extension of the

Type II burst nor the same as the Type IV burst. It is a distinctive type of burst and may be called "Microwave

burst" or "M-type" burst. In comparison with the current

classification of bursts at microwave frequency, short lived

SD (Simple and Distinct) and CD (Complex and Distinct)

295
bursts whose durations are less than about 10 min seem to

be the "M-type" bursts, while long lived CD bursts might

be Type IV bursts. (Met. Abst. 1 1L -97. )- -Author's abstract.

D-812 Tanaka, Haruo; Kakinuma, T. ; Jindo, Hidehiko and Taka

yanagi, Toshio, Equipment for the observation of solar

noise at 3750 Mc. Nagoya. Univ. Research Inst, of Atmospherics, Proceedings, 1:71-85, Jan. 1953. 23 figs.

,

2 photos, 5 refs. , eqs. DWB--Equipment for measuring 8

cm radio waves from the sun (solar noise) was designed

by the authors in 1950 and tested by actual observations

for 600 hrs in 1951, then modified and used for systematic

observations from Nov. 1951 through 1952 with alterations

in Aug. 1952. The method is similar to that of R.H.DICKE

(1946). Details of construction of aerials, modulator, balanced frequency converter, amplifiers, synchronous rectifiers, output, power supply, signal generator and calibrations are given in text and illustrations. Theoretical calculations of output fluctuations also given. (Met. Abst.

12. 1-113. )--M.R.

D-813 Tanaka, H. and Kakinuma, T. , Equipment under construction for locating sources of solar noise at 4000 Mc. Nagoya.

Univ. Research Inst, of Atmospherics, Proceedings, 1:89,

Jan. 1953. photo. DWB--An interferometer with 5 aerials

was constructed beginning in May 1952. Aerials are placed

at 6 m intervals in an E-W direction. Test observations

were to be performed in April 1953, by scanning the sun

"stripwise as it passes through the aerial pattern." (Met.

Abst. 12. 1-114. )-M.R.

D-814 Tanaka, H. and Kakinuma, T. , Observations of solar radio

noise at 3750 Mc. Nagoya. Univ. Research Inst, of Atmospherics, Proceedings, 1:103-107, Jan. 1953. 2 figs. , 2

tables. DWB--Summary of data from station near Nagoya for

the Sub-Committee for Worldwide Network on Solar Radio

Emission of the U. R.S.I. Test observations from April-July

1951 and daily values from Nov. 1951 to Jan. 1953 are given

on graphs, and data for outstanding occurrences in tables

(starting time, duration, type, maximum intensity and time,

and radio fadeouts). (Met. Abst. 9A-41. )--M. R.

D-815 Tanaka, H. and Kakinuma, T. , The most intense burst of

solar radio emission observed on Feb. 23. 1956. Nagoya.

Univ. Research Inst, of Atmospherics, Proceedings, 4:74-

77, Dec. 1956. 3 figs. , ref. DWB--A violent outburst of

solar radio emission was observed on Feb. 23, 1956. A

perfect record of the intensity was successfully obtained by

296
3750 and 9400 Mc/s radiometers, together with a drift

curve taken by an 8 element interferometer at 4000 Mc/s.

The maximum intensity was 225 and 141 times as large as

that of the quiet -sun radiation for 3750 and 9400 Mc/s ra- dio flux density, respectively. The position of the radio

source at 4000 Mc/s slightly moved during the burst. The

most probable E-W width of the radio source during the

burst is 3 min of arc, which corresponds to the maximum

effective temperature of about 5 X 10° K. (Met. Abst.

9A- 136. ) -Authors' abstract.

D-816 Tanaka, H. and Kakinuma, T. , Observations of solar

radio emission at microwave frequencies. Nagoya Univ.

Research Inst, of Atmospherics, Proceedings, 5:81-89,

March 1958. 12 figs. , 3 tables, 6 refs. DWB--Outline of

the equipment used for radio observations at Toyokawa station which are in operation since the beginning of IGY, is

described together with the method of tabulation. Percentage variation of the S component versus frequency is calculated for the first half year period of IGY, which shows

a peak near 4000 Mc/s and there are many cases where the

sense of polarization reverses between 3750 and 9400

Mc/s. Experiment has been made for detecting linear polarization at a frequency of 3750 + 5 Mc/s, but we have

yet no data to show the existence of linear polarization for

both S component and outstanding occurrences. (Met. Abst.

unpub. )- -Authors' abstract.

D-817 Tandberg-Hanssen, Einar (Inst, of Theoretical Astrophysics, Oslo and Mt. Wilson and Palomar Obs. ), On the cor- relation between radio frequency radiation from the sun and

solar activity. Astrophysical Journal, Chicago, 121(2):

367-375, March 1955. 7 figs. , 2 tables, 11 refs. (Also

issued as Oslo. Universitet. Institutt for Teoretisk Astrofysikk, Reprint, No. 10.) DLC --An investigation is made

of the correlation between radio frequency radiation from

the sun and solar activity, sunspots, prominences, and geomagnetic disturbances. The difference in observed directivity and intensity of the radiation at different frequencies is

explained by the reflection conditions in the sun's atmosphere. A distinction is made between radio noise active

and radio noise inactive sunspots. (Met. Abst. 9A-97. ) --Author's abstract.

D-818 Tandberg-Hanssen, E. , On the correlation between solar

flares and radio bursts. Astrophysics Norvegica, Oslo,

6(2), Oct. 1957. 25 p. 2 figs. , 5 tables, 8 refs. DLC--

297
Some 700 cases of time coincidences between flares and —

presumably randomly polarized — radio bursts on 200 Mc/s

have been analyzed to study the correlation between flare

importance and radio bursts. It is found that as a general

rule the correlation increases greatly with the importance

of the flares. Bright flares occur, however, at times when

there is no indication of excess radio radiation, and strong

radio bursts are not infrequently observed at times when

there is no excess Hx

radiation. One is led to conclude

that radio bursts are not to be considered as flare induced

phenomena, but that flares and radio bursts are but two

manifestations of a common disturbance. (Met. Abst. un- pub. )- -Author's abstract.

D-819 Tandon, Jagdish Narain (Physics Dept. , Univ. of Delhi),

Radio astronomy. Science and Culture, Calcutta, 22(1):4-

11, July 1956. 2 figs. , 2 tables, 27 refs. DLC--A review

of discovery by JANSKY (1931) of radio waves from space,

and subsequent discoveries regarding sources of these ra- diations, uses of the information in astrophysics, ionospheric physics and astronomy, and other aspects of radio

astronomy (meteor trail investigations, interstellar hydrogen, solar radio radiation, echoes from ionosphere, etc.).

It is demonstrated how this discovery has opened a window

into space that is 100 times as wide (with respect to the v,

m spectrum) as was possible with visible or photographic

radiation. (Met. Abst. 9A-137. )--M. R.

D-820 Taubenheim, Jens (Berlin-Adlershof), Messunqen der Absorption von Kurzwellen in der Ionosphare. (Measurement

of the absorption of short waves in the ionosphere. ) Freiberger Forschungshefte, Ser. C, Geophysik, No. 29:1-18,

Oct. 1956 (issued Berlin, Akademie Verlag). 8 figs. , 22

refs. , 10 eqs. DWB--A review of recent knowledge concerning absorption of short radio waves in the various ionospheric layers, methods of measurement, the relation to

propagation and the relation of propagation to knowledge of

the electrical properties of these layers of the upper atmosphere. Diurnal, seasonal, sunspot cycles and eclipse effects or variations are discussed and illustrated. Focussing and de-focussing are illustrated schematically. (Met.

Abst. 10. 11-136. )-M.R.

D-821 Taubenheim, J. , Incoherency of pulse echoes and the measurement of ionospheric absorption. Journal of Atmospheric

and Terrestrial Physics, London, 18(2/3): 147-151, June

1960. 3 figs. , 6 refs. , 13 eqs. DLC--The presence of incoherently scattered energy in the h. f. pulse echoes from

298
the ionosphere gives rise to errors in the absorption value

determined from the median echo amplitude. These errors are larger for the second order than for the first order echo.

The calculations are confirmed by experimental results.

(Met. Abst. 11. 12-440. ) -Author's abstract.

D-822 Taylor, Eloise W. , Absorption of radio waves reflected at

vertical incidence as a function of the sun's zenith angle.

U. S. National Bureau of Standards, Journal of Research,

41(12):575-579, Dec. 1948. 2 figs. , 3 tables, 2 eqs. DWB

--The diurnal variation of ionospheric absorption is related

to the sun's zenith angle. The absorption values for this

study were obtained from the continuous automatic field intensity recordings made at the Central Radio Propagation

Laboratory on two frequencies. Because of proximity of the

receiving station to the transmitting station, reflections are obtained at nearly normal incidence. An analysis of data

covering a period of 3 yrs indicates that little error is introduced by assuming a linear dependence of absorption upon

the cosine of the sun's zenith angle. (Met. Abst. 10. 11-

137. ) --Author's abstract.

D-823 Taylor, Paul B. and Engler, Nicholas A. , Charts of correc - tions to radar observations for refraction by terrestrial atmospheres. Dayton, Ohio. Univ. Research Institute. Contract AF 33(616)-5438, Research Report 427-71, Feb. 1960.

139 p. 4 figs. , 100 charts, 4 tables, 15 refs. , numerous

eqs. (U. S. Wright Air Development Center, WADC Technical Report 59-619). DWB (M(051) U589ch) -There are presented in chart form corrections for atmospheric refraction

to observations of range and angular altitude of targets observed by electromagnetic radiation at either visual or radar

wavelengths. These corrections have been computed for

16 type atmospheres above a spherical earth. In these atmospheres the index of refraction attenuates exponentially

with height. The type atmospheres cover a range of base

indices and exponential attenuation rates. Tabulations of

the computations upon which the charts are based are available upon application to the Project Engineer. These tabulations list A- 1 , n - 1 and sin A in addition to the quantities used directly in plotting. The original charts were

prepared on paper having five divisions to the half centimeter. Copies of these original charts are also available.

The charts appearing in this report are reduced copies of

vellum tracings of the original charts, the tracings having

two divisions to the centimeter. —Authors' abstract.

299
D-824 Taylor, William C. (Lockheed Missiles and Space Div. ),

Analysis and prediction of radio signal interference effects

due to ionized layer around a re-entry vehicle. Planetary

and Space Science, N. Y. , 7:286-300, July 1961. 12 figs.,

21 refs. , 11 eqs. DWB, DLC—Effect of thermal ionization

upon radio signals from a re-entering space vehicle are discussed in terms of determination and particle density, plasma wave interaction and plasma properties, and collision

frequency. Conclusions are drawn for radio signals at 200

and at 10, 000 Mc/s. It is shown that the plasma effects

can be controlled by increased frequency during re-entry.

--W. N.

D-825 Taylor, W. C. (Lockheed Aircraft Corp. Missiles and

Space Div. , Sunnyvale, Calif. ), Analysis of radio signal

interference effects due to ionized layer around a re-entry

vehicle. Planetary and Space Science, N. Y. , 6:1-9, June

1961. 7 figs. , ref. , 4 eqs. DWB--Transmission problems

at 200 Mc/s during re-entry are discussed. Methods of

predictions and calculations under given conditions are shown to agree satisfactorily with practical tests. --W. N.

D-826 Theissing, H. H. and Caplan, P. J. , Atmospheric attenuation of solar millimeter wave radiation. Journal of Applied

Physics, 27(5): 538-543, May 1956. -Measurements of water

vapor absorption at around 1 mm compared with van VleckWeisskopf theoretical equation. --CSIRO Abstract.

D-827 Theissing, H. H. and Caplan, P. J. , Measurement of solar

millimeter spectrum. Optical Society of America, Journal,

46(ll):971-978, Nov. 1956. -Used a thermal detector, and

filters of woven copper wire mesh. The observed spectrum

agreed with a Raleigh-Jeans curve, allowing for van Vleck's

atmospheric attenuation data. --CSIRO Abstract.

D-828 Thomas, J. A. (Univ. of Queensland, Brisbane) and Hibberd, F. H. (Univ. of New England, Australia), Satellite

Doppler measurements and the ionosphere. Journal of Atmospheric and Terrestrial Physics, London, 13(3/4) :376-

379, Feb. 1959. fig. , 2 refs. , 3 eqs. DLC--An outline of

the method of an analysis of the effect of the ionosphere on

the simultaneous Doppler frequency shifts of the 20 and 40

Mc/s signals from Sputnik I is presented. (Met. Abst.

11. 12-377. )-O.T.

i

1

300
D-829 Thomas, J. O. and Robbins, A. R. (both. Cavendish Lab.

Cambridge), Movements in the F2 layer of the ionosphere

during some solar eclipses. (In: Solar eclipses and the

ionosphere: a symposium. . . ed. by W. J. G. Beynon and

G.M.Brown. London, Pergamon, 1956. p. 94-101. 4 figs.,

table, 10 refs. , 3 eqs. DWB--Five different sets of ionosphere soundings made during eclipses have been analyzed

in an attempt to see whether vertical transport of electrons

plays an important part in the F2 layer during an eclipse.

The assumption was made that the rates of production and

loss of electrons were those tentatively suggested by RATCLIFFE et al. (1956). It has been found that the five sets

of observations lead to fairly similar conclusions. Vertical

movements of importance seem to have occurred during the

eclipses. Their possible causes are considered. (Met.

Abst. 9.6-269.) -Authors' abstract.

D-830 Thompson, A. R. and Maxwell, A. , Solar radio bursts and

low energy cosmic rays. Nature, London, 185(4706) :89 -90,

Jan. 9, 1960. fig. , table, 10 refs. DWB, DLC--This paper

considers the radio spectral observations of the sun, and

from this elucidates the origin of the solar protons of ener- gies 30-300 MeV and their relation to solar radio bursts,

flares, and terrestrial disturbances. The data consists of

a continuous record of solar radio bursts obtained from sunrise to sunset for the past three years at the Harvard Radio

Astronomy Station, Ft. Davis, Texas, with sweep frequency

receivers covering the range 25-580 Mc/s. (Met. Abst.

11. 12-60. )-I.S.

D-831 Tischer, F. J. , Propagation-Doppler effect in space communications. Institute of Radio Engineers, Proceedings,

48(4): 570-574, April 1960. 3 figs. , 4 refs. , 51 eqs. DLC

--A Doppler equation, derived by field theory, is presented

in this investigation of the effect of a nonhomogeneous medium in the flight direction. Subsequently, the derived re- lations are used to consider typical deviations from the re- gular Doppler shift due to the influence of the propagation

phenomena. --From author's text.

D-832 Trexler, James H. , Lunar radio echoes. Institute of Radio

Engineers, N. Y. , Proceedings, 46(1): 286-292, Jan. 1958.

13 figs. , 21 refs. DLC--High power radars at the Naval Research Laboratory have been used to study the reflecting

properties of the earth's moon. Experimental work over the

last six years at frequencies in the 30 to 3000 Mc band has

revealed a lunar surface phenomenon which produces a

"highlight." Measurements made at 198 Mc have shown

that more than 50% of the echo energy is reflected in the

301
first 50 microsecond after the leading edge of a short incident pulse contacts the moon. This fortunate situation permits many interesting astronomical observations and suggests the use of wide band communication signals in a circuit using the moon as a passive relay. Many types of

modulation have been successfully passed over the lunar

circuit, including amplitude modulation by voice. (Met.

Abst. unpub. )--Author's abstract.

D-833 Triskova, Ludmila (Prague), Ionisation durch Erdsatelliten. (Ionization by earth satellites. ) Beitrage zur Geophysik, Leipzig, 68(4): 246-249, 1959. 6 refs. , 5 eqs.

German and English summaries p. 246. DWB, DLC--It was

experimentally found that frequencies higher than the MUF

are reflected by the space ionized by an artificial earth

satellite. The process of ionization is investigated. Especially ionization by molecules accelerated by collision

with the satellite is considered and this process appears

probable. (Met. Abst. 11D-144. )--Author's abstract.

D-834 Twiss, R.Q. (C.S.I. R.O., Univ. Grounds, Chippendale,

N. S. W. ), Radiation transfer and the possibility of negative absorption in radio astronomy. Australian Journal of

Physics, Melbourne, 11(4): 564-579, Dec. 1958. 20 refs.,

55 eqs. DLC --Stimulated transitions are relatively enor- mously more probable at radio than at optical frequencies

and it is this which makes it possible for negative absorption to arise at radio wavelengths when the medium will behave like an amplifier to the incident radiation. A necessary condition for the existence of this phenomenon is that

the kinetic energy distribution Ft. 1

/) of the radiating electrons be markedly non-thermal with an appreciable excess

of high energy electrons such that 3F/ 3 1\ is positive

over a finite range of the kinetic energy .^ , However, this

condition is not sufficient, since it is shown that an electron gas in which free-free transitions provide the dominant

radiation process can never exhibit negative absorption

whatever the form of F( \), and it is further necessary that

the stimulated transition probability should have a maximum

at some finite value of the kinetic energy, the most favorable case occurring when this maximum is a sharp one at

the value of ^at which 3 F/ d ^ has a positive maximum.

These conditions can both be met in principle for the cases

in which the dominant radiation process is due (a) to Cerenkov effect, (b) to gyro radiation by non-relativistic electrons, (c) to synchrotron type radiation by highly relativistic electrons, and it is shown that negative absorption can

arise in all these cases; the relevance of these results to

radio astronomy is discussed briefly. (Met. Abst. 12. 6-165. ) --Author's abstract.

302
D-835 Tyas, J. P.I. ; Franklin, C.A. and Molozzi, A. R. f Measurement of cosmic noise at low frequencies above the ion - osphere. Nature, London, 184(4689): 785-786, Sept. 12,

1959. 9 refs. DWB--The paper reports a 2-15 Mc/s swept

frequency ionosphere sounder, being designed at present

under the auspices of the Canadian Defence Research Bd.

,

in cooperation with the National Aeronautics and Space Administration, to be launched as an Earth satellite. The

practicability of this device for measurement of cosmic

noise is discussed. (Met. Abst. 11. 12-44. )--I. S.

D-836 U. S. Dept. of the Army. Army Library, Guided missiles,

rockets and artificial satellites (including Project Vanguard): a selected list of titles . Its Special Bibliography,

No. 11, Jan. 23, 1957. 153 p. "Current companion volume to its Special Bibliography, No. 4 (Guided Missiles),

April 20, 1956. " DWB-Briefly- or non-annotated reference

material is arranged in alphabetical order by title within

major and subject groups, under Sec. VI. Missiles and

Rockets (by type). Pt. E (Experimental and Specialized

Vehicles) contains references to Aerobee Rockets (p. 48),

ASP (Atmospheric Sounding Projectile) (p. 48), Viking

(p. 52). Artificial Satellites are covered in Pt. II (IGY

program, p. 130; Project Vanguard, p. 131; other satellite projects, p. 145). Scientific applications of satellites are covered on p. 151. At least 50 papers or books of interest to meteorologists will be found in this section. No

author or subject index is provided. (Met. Abst. 8. 8-81. ) --M. R.

D-837 Utah. University, Physical properties of the upper atmosphere. Contract W19-122 ac-15. Progress Report, No. 17,

May 31, 1952, and Final Report for the Contract. Pub.

July 30, 1952. 50 p. 8 figs. , table, refs. DWB--An administrative report outlining the activities of the project

which was mainly concerned with the development of airborne and ground equipment for the study of electromagnetic

waves at various altitudes by means of V-2 rockets and aero- bees. The method of attack was several times modified during the development of the work. Great care was taken in

the construction of an antenna adequate from both the transmission and aerodynamical points of view. The desired

data about ion density transmission constants, etc. , were

not obtained since all the rockets misfired with the exception of one whose beacon failed shortly after landing. Circuit schemes for the developed equipment are included.

(Met. Abst. 6. 6-74. )--A. A.

303
D-838 Uyeda, Hiroyuki; Shibata, Hisashi; Mambo, Masayoshi

(all, Radio Res. Labs. ) and Ishida, Tadashi (Kanto Radio

Regulatory Board), On the reception of radio waves from

Sputnik I. Japan. Science Council. Ionosphere Research

Committee, Report of Ionosphere Research in Japan, 12(1):

37-39, 1958. 2 figs. DWB, DLC--A short note analyzing

the satellite's orbits obtained from the data observed at the

Monitoring Division, Kuiki Radio Regulatory Bureau, Ministry of Posts & Telecommunications and from the ephemeris

given by the Smithsonian Astrophysical Observatory. The

regions of reception analyzed on the normal propagation by

F2 and Es layer reflections, and graphically represented,

are divided into two regions. Region I corresponds to the

region in which the satellite is in flight lower than the

height of points of maximum electron density in the F2 layer, and region II corresponds to the other region in which

the satellite is in flight higher than the height of points of

maximum electron density in the F2 layer. An analysis of

both regions is presented. (Met. Abst. 11E-160. )--I. S.

D-839 Van Allen, James A. (ed. ), Scientific uses of earth satellites . Ann Arbor, Univ. of Michigan Press, 1956. 316 p.

figs. , tables, bibliogs. throughout. Price: $10. 00. DWB--

A compilation of 33 of the papers presented at the Upper

Atmosphere Rocket Research Panel meeting at Ann Arbor,

Mich, on Jan. 26-27, 1956. The papers are devoted to detailed, specific proposals for use of satellites in measuring temperature, density, air-drag, pressure, radiative heat

transfer, visibility, hydrogen in space; UV, auroral and

cosmic ray flux; geomagnetic field, ionospheric structure,

meteoric drag, interplanetary dust, radio propagation, etc.,

as well as the performance of the satellite itself. (Met.

Abst. 8.4-6.)-M.R.

D-840 Van Allen, J. A. ; Ludwig, G.H. ; Ray, E. C. and Mcllwain,

C. E. , Observation of high intensity radiation by satellites

1958 Alpha and Gamma (1958) . 19 p. 8 figs: , table. Mimeo.

"Assisted by U. S. /I. G. Y. Project 32. 1 of the Nat'l. Academy of Sciences and the Nat'l. Science Foundation." —A preliminary report is given of the results obtained by artificial

earth satellites Explorers I and III in measurements of radiation intensities and of several geophysical effects, by means

of a single Geiger Mueller tube, a scaling circuit for reducing the number of pulses to be worked with, and telemetering

systems used for transmitting the scalar output to the ground

receiving stations. (Met. Abst. 10. 10-133. )--N. N.

304
D-841 Van Bladel, J. (Univ. of Wash. ), Les applications du

radar a l'astronomie et a la meteoroloqie. (Applications of

radar to astronomy and meteorology. ) Pref. byM.P.Lejay,

Paris, Gauthier-Villars, 1955. 147 p. 55 figs. , 6 tables,

196 refs. --This monograph presents a complete coverage of

the manifold uses of radar in observing astronomical and

meteorological objectives such as the sun, moon, planets,

zodiacal light, meteorites, auroras, lightning, precipitation, snow, turbulence, thunderstorms, tornadoes and

clouds. The six major sections cover: 1. General theory,

design and operation of the equipment and the electromagnetic waves; 2. Diffusion by opaque spheres and echoes

from heavenly bodies; 3. Diffusion from ionized trails

from meteors, meteor showers, effect of upper winds, re- combination, ionization variations, sporadic ionization;

4. Detection of auroras, auroral ionization and lightning;

5. Detection of precipitation, physical basis, quantitative

and qualitative statics of precipitation and turbulence, upper bands; 6. Rawinsondes for obtaining upper air winds

with primary and secondary radar. A very complete bibliography, including material published through 1954 is

appended. Many illustrations from recent publications are included. (Met. Abst. 7. 1-25. )--M. R.

D-842 Van Isacker, J. , La scintillation des etoiles . (The scintillation of stars. ) Belgium. Institut Royal Meteorologique,

Publications, Ser. B, No. 8, 1953. 110 p. figs. , tables,

17 refs. , eqs. DWB--A statistical theory is developed for

determining angular distribution, covariant and spectrum of

starlight intensity as functions of the variation of refractive

index in the atmospheric layers. This method of computation makes it possible to derive upper tropospheric temperatures from star scintillation measurements. The study includes an analysis of the observations made in Ireland by

BUTLER. It is shown how the theory can be applied to scintillation of radio stars and to fading of radio waves reflected by the ionosphere. (Met. Abst. 5. 11-214. )--G.T.

D-843 van Sabben, D. , Relationship between radio propagation

disturbance, geomagnetic activity and solar noise. Journal

of Atmospheric and Terrestrial Physics, 3(4): 194-199, May

1953. 3 figs. DWB--A radio propagation disturbance index

I is derived and its variations in circuit New York-Amsterdam compared with variations of geomagnetic K. Close

agreement is found, I having a mean lag of 7 hrs behind K.

A nonrecurrent magnetic storm was generally preceded by

an increased flux of radio noise, average interval 2 days.

(Met. Abst. 5. 1-118.)-C.E.P.B.

305
D-844 Vassy, E. , La haute atmosphere. (The upper atmosphere.

)

La Meteorologie, Paris, 4th Ser. , No. 35:185-194, July/

Sept. 1954. 12 figs. DWB--Review of different indirect

methods for obtaining information on the high atmosphere

(radio and sound propagation, meteors, ozone, twilight

airglow and auroral data), and direct methods used since

the war (rockets) to obtain density, temperature, chemical

composition, ozone and mass spectrometer data. Measurement of electrical properties by means of (a) UHF; (b) the

U.S. Naval Research Laboratory (NRL) method using two

figures, 2. 34 Mc and 25. 6 Mc, or the sixth harmonic of

the first, to determine ionization at 80-160 km; (c) the

Langmuir method which determines that no electrons exist

below 70 km, although + and — ions occur at 60 km; and

(d) Doppler method are described. (Met. Abst. 9. 9-107. ) --M.R.

D-845 Vassy, E. , Les satellites artificiels, leur interet pour

1' etude de 1 'atmosphere. (Artificial satellites: their importance in the study of the atmosphere. ) La Meteorologie,

Paris, Ser. 4, No. 40:283-290, Oct. /Dec. 1955. 3 figs.

,

eqs. English and Spanish summaries p. 283. DWB--The

writer shows that it is necessary for some types of research

to have a means of rapid high-altitude exploration along a meridian. He reviews solar emission in the ultraviolet

range, X-radiation, charged particles causing northern

lights and variations in the earth's magnetic field, in cos- mic radiation and their effect.s on the upper atmosphere. It is demonstrated that it is possible to make artificial satellites. Summary report of the American "MOUSE" Project.

(Met. Abst. 8.4-58. ) -Author's abstract.

D-846 Vassy, E. , Radionaviqation et telequidaqe a qrande distance. (Long distance radio navigation and remote control.)

Annales des Telecommunications, Paris, 14(9/10): 256-260,

Sept. /Oct. 1959. 5 figs. , 5 refs. , eqs. DLC -.-Statement

of a theoretical method relating to a hyperbolic system working through phase lag, which proves that it is possible to

take advantage of the ionosphere provided that the chosen

frequencies correspond to a level of the curve h'f where h'

is the apparent height or virtual height of the trajectory and

f the exploring frequency. The author investigates two

cases: that of combined direct and ionospheric waves in

the case of RANA (see: L'Onde Electrique, Paris, 1955, p.

319) and that of ionospheric wave only. The choice of the

frequencies permitting theoretical functioning of long distance radio navigation is determined, and the disturbing influence of the ionosphere on the phase is examined. The ex- perimental process is described and the results obtained are

stated. (Met. Abst. 11. 8-107. )--A. V.

306
D-847 Vassy, E. , L 'emission radioelectrique des satellites

artificiels. Applications a la connaissance de 1 'ionosphere. (Radio transmission from artificial satellites. Applications to the knowledge of the ionosphere.) L'Onde

Electrique, Paris, 39(388/389):647-653, July/Aug. 1959.

8 figs. , table. French and English summaries. DLC--The

radio features of the Soviet and U. S. artificial satellites are summarized. A description is then given of investigations of the properties of the upper atmosphere based on

the simple reception of a transmitted radio signal without

knowledge of the code. A report is made of the methods

to determine the air density of the upper atmosphere, using

the Doppler-Fizeau effect, radio interferometry, the Faraday effect and refractive waves. The author comments on

these various methods and shows their great utility. (Met.

Abst. 11.5-166. )--A.V. and author's abstract.

D-848 Vauquois, Bernard; Coupiac, Pierre and Laffineur, Marius,

Etude experimentale des orages radioelectriques solaires.

(Experimental study of radioelectric solar storms. ) Academie des Sciences, Paris, Comptes Rendus, 237(25) : 1630-

1632, Dec. 21, 1953. fig. , 5 refs. DLC--The results of

observations of simple radioelectric storms of solar origin

on 5 occasions in 1952 and 1953 at Sydney, Cambridge,

Nera, and Meudon indicate that there is a dissymmetry

which depends on the longitude of the sunspots and on the

wavelength. (Met. Abst. 9A-42.)-M. R.

D-849 Veldkamp. J. , De eerste Amerikaanse kunstmaan. (The

first American artificial satellite. ) Hemel en Dampkring,

The Hague, 56(7/8): 147-149, July/Aug. 1958. 3 figs.

DWB, DLC-Description of the first U.S. satellite 1958 *,

sent up on Jan. 31, 1958 at Cape Canaveral. Statement

of the transmitters and observation methods, followed by

a commentary of the research by means of satellites. (Met.

Abst. 11J-183.)--A.V.

D-850 Veldkamp, J. and van Sabben, D. (both, R. Netherlands

Met. Inst. , De Bilt), On the current system of solar flare

effects . Journal of Atmospheric and Terrestrial Physics,

London, 18(2/3): 192-202, June 1960. 7 figs. , 16 refs.

,

6 eqs. DLC--The electric current system responsible for

the great solar flare effect (s. f. e. ) of March 23, 1958, is

compared with the currents of the normal daily variation of

the geomagnetic field. Whereas the standard Sq currents

are symmetric with respect to the geographic equator, the

pattern of the currents of the s. f. e. , as well as that of

the currents of the normal daily variation at the time of

307
the s. f. e. are controlled by the magnetic equator. The

same result is found by a re -examination of selected s. f. e.s published in the IATME Bulletins nos. 12f and 12h. It is

shown that the s. f. e. currents must flow in a region where

the disappearance of electrons follows an attachment law.

The decrease of the s. f. e. leads to a loss coefficient

= 5 X l-"

4* sec"-*-, which compares with the known value

for the D layer. (Met. Abst. 11. 12-104. ) -Authors' abstract.

D-851 Venugopal, V. R. (Kodaikanal Observ. , Kodaikanal), Sun- rise effect in the F region of the ionosphere over Kodaikanal . Indian Journal of Meteorology and Geophysics, Delhi, 10(3):

325-330, July 1959. fig. , table, 8 refs. DWB, DLC--The

sunrise effect in the F region of the ionosphere over Kodaikanal has been studied. It is found that' the effect occurs

about an hour after the moment of sunrise for visible rays

in the layer and a few minutes before ground sunrise. This

result is compared with those obtained at other places. The

delay in the occurrence of the sunrise effect is believed to

be due to the absorption of the solar ionizing radiation by

the ionospheric layers lying to the east of the observing

station. (Met. Abst. 11D-146. )--Author's abstract.

D-852 Vilbig, Friedrich (Communication Sciences Lab. , Air Force

Cambridge Research Center), Global communication using

passive or active satellite relay stations. Advances in the

Astronautical Sciences, N. Y. , Vol. 5, 1959, issued 1960.

p. 251-260. 9 figs. , 2 refs. , 12 eqs. DWB (629. 1388

A512pro), DLC (QB1. A26)--The limitations of present day

long distance communication links are compared with the

limitations of links which might use passive or active satellite relay stations. The paper is largely concerned with

orbital paths and the number and distribution of satellites

required for several possible communication systems. A

probability calculation showing the distribution and number

of satellites required for line-of-sight interception at any

earth point is also given. (Met. Abst. 11. 12-490. ) --Author's abstract.

D-853 Viterbi, A. J. (Jet Propulsion Lab. , Calif. Inst, of Technology, Pasadena), Design technigues for space television. Advances in the Astronautical Sciences, N. Y. , Vol. 5, 1959,

issued 1960. p. 291-305. 7 figs. , 3 refs. , 40 eqs. DWB

(629. 1388 A512pro), DLC (QB1. A26)--The basis for establishing a television system for obtaining visual images of

the planets is outlined. This entails consideration of the

distances involved, signal levels and noise environment. An

FM-PM communication system is described and design re- strictions formulated. The problem is then illustrated by an

308
example involving transmission of a television image from

the vicinity of Venus. (Met. Abst. 11. 12-489. )--Author's

abstract.

D-854 Vitkevich, V. V. , Issledovanie ionosfernykh neodnorodnostei radioastronomicheskimi metodami. (Investigation of

ionospheric inhomogeneities by the methods of radioastronomy. ) Radiotekhnika i Elektronika, 3(4):478-486, April

1958. 2 refs. DLC--The method based on the radio emission of "radio stars " is used to study electronic inhomogeneties in the ionosphere. The size and electronic concentration of large inhomogeneties are calculated from data

on irregularities in vertical ionospheric refraction. Data

are supplied on the irregularities in horizontal radio refraction and also on the electronic irregularities which confuse the interference picture. --R. M.

D-855 Vitkevich, V.V. ; Gorelova, M.V. and Lozinskaia, T. A.

(all, Acad. Sci. , U.S.S.R.), The spectrum of peaks in

solar emission. Soviet Astronomy AJf N. Y. , 3(4):626-

627, Jan. /Feb. 1960. fig., 6 refs. DLC. Transl. of

Spektr pichkov radioizlucheniia Solntsa, Astronomicheskii

Zhurnal, Moscow, 36(4): 641 -642, July/Aug. 1959. DLC--

Two types of short duration bursts of solar radio frequency

emission are described: narrow band width peaks with a band width ranging to 5 Mc, and wide banded peaks with a band width of the order of 12-15 Mc. (Met. Abst. 11L-90.

)

--Authors' abstract.

D-856 Bogelman, Joseph H. , Propagation and communications

problems in space. Institute of Radio Engineers, N. Y.

,

Proceedings, 48(4): 567-569, April 1960. 3 figs. , 2 tables.

DLC --The problems of propagation and communications arising from landings on the Moon, Venus, or Mars are treated

in terms of the characteristics required for the communication system to achieve data transfer between parties on the

surface of these bodies and the communications problems

arising in the transfer of information from these bodies back

to the Earth. Consideration is given to Doppler shift, Faraday rotation, tracking and stabilization of antennas, and

ground network requirements. The problems of communications between vehicles in space in terms of signal acquisition and antenna orientation and tracking are described.

(Met. Abst. 11. 12-480. )--Author's abstract.

309
I

D-857 Voigt, H. H. , Identifizierunq der kosmischen Radiostrahluncrsquellen mit optischen Obiekten. (Identification of

cosmic radio sources with optical objects. ) Naturwissenschaften, 42(5): 115-119, March 1, 1955. 2 figs. , 10 refs.

DWB--The two "windows" in the atmosphere are 3000-

30, 000 A (optical) and 1 cm-20 m. Radio radiators are defined as objects which emit radio radiation far exceeding

the long wave extension of thermal radiation. Types of

nonradiating and radiating optical objects are listed. Extragalactic emissions from Crab nebula, Cassiopeia, Cyghus, etc. , and emissions from the Milky Way are discussed. (Met. Abst. 9A-98.)--C.E.P.B.

D-858 Voigt, H. H. , Radioquellen ausserhalb der Milchstrasse.

(Radio sources outside the Milky Way.) Umschau, 55(24):

744-746, Dec. 15, 1955. 2 figs. DLC--So far radio emission has only been found from spiral Sc nebulas such as

Andromeda, some colliding star swarms such as Cygnus A

(very strong), and an elliptical nebula emitting a "plume"

of unknown composition. The sources are probably turbulent gas clouds. (Met. Abst. 9A-99. )--C.E.P. B.

D-859 Voigt, H. H. , Radiostrahlunq und Sonnenaktivitat. (Radio

radiation and solar activity. ) Umschau, Frankfurt a. M.

,

56(17):525, Sept. 1, 1956. fig. DLC--The correlation between solar activity and solar radio radiation is much closer

for frequencies above 600 MHz (50 cm) than in the meter

wave region. On 2800 MHz (10.7 cm), E.TANDBERGHANSSEN found a very close relation with monthly sunspot

relative numbers Jan. 1950-April 1951. He distinguishes

between active and inactive spots. (Met. Abst. 8. 1-227.

)

--C E. P. B.

D-860 Voigt, H. H. , Das "optische" und das "Radio-Fenster" in

der Astronomie . (The optical and radio windows in astronomy. ) Umschau, Frankfurt a. M. , 56(ll):323-325, June

1, 1956. 2 figs. DLC--The atmosphere is transparent to

electromagnetic waves from 3000 A to near infrared and

from < 1 cm to 20 m; the latter also pass through clouds.

The intensities and wave lengths from sources at 1 to 10°

A are shown; for the sun the maximum is approximately in

the visible range. Problems of stellar emission are discussed; radio waves are essentially different in origin

from light rays. (Met. Abst. 8. 1-223. )--C. E.P. B.

310
D-861 Voigt, H. H. , Die 21-cm-Linie: neue Moglichkeiten and

Ergebnisse in der Astronomie. 1, Beobachtungen innerhalb

unserer Milchstrasse. (The 21-cm line: new possibilities

and results in astronomy, Pt. 1, Observations within our Galaxy.) Umschau, 59(15): 452-455, Aug. 1959. 3 figs.

Pt. 2. Beobachtungen an aussergalaktischen Obiekten.

(Pt. 2, Observations on outer galactic objects. ) Ibid.

,

59(16):494-496f Aug. 15, 1959. photo, table, 6refs.DLC

-•In this first review paper, the author discusses the physical characteristics of the 21 cm line, the celestial mechanics of our galactic system, the systematic analysis of

the 21 cm line along the galactic plane and the demonstration of the spiral structure of galactic system; detailed

structure of the spiral arms including hydrogen atmosphere

and clouds, interaction between interstellar hydrogen and

pleiades, etc. ; physics of interstellar matter; the Magellanic clouds including their radial velocities, the Andromeda cloud; cloud nebula and the red displacement. The

second part of the article reports the details of observations such as the Magellanic and Andromeda clouds, the

red shift, etc. (Met. Abst. 11. 9-112. )-I.L. D.

D-862 Volland, Hans, Die Freguenzabhangigkeit der Sonnenerup- tionseffekte im La'ngstwellengebiet. (Frequency dependence of solar flare effects in the region of very long waves.)

Archiv der Elektrischen Ubertragung, Stuttgart, 13(10):443-

448, Oct. 1959. 11 figs. , 7 refs. German and English

summaries p. 443. DLC—Measurements of field strength

of the transmitters GBR (16 kc/s), GBZ (19. 6 kc/s) and

GIY 20 (51. 95 kc/s), made in the Heinrich-Hertz Institut

in Berlin-Charlottenburg during solar flares, show positive

and negative field anomalies, dependent on frequency, time

of day, and year. These are explained as interferences between ground wave and rays reflected from the ionosphere.

It is assumed that the height of reflection decreases during

a solar flare. The median height of reflection is between

69 and 76 km for 16 kc/s. It decreases down to 12 km during a solar flare. The same model can explain the change

of the frequency spectrum of atmospherics during a solar

flare. (Met. Abst. 11E-163. ) -Author's abstract.

D-863 Von Kluber, H. , Beobachtungen der Sonnenfinsternis vom

25 Februar 1952 im Sudan. (Observations of the solar e- clipse of Feb. 25, 1952 in the Sudan. ) Naturwissenschaften,

39(9): 199-206, May 1, 1952. 9 figs. , 10 refs. DWB--A

brief introduction describes the physics of the sun and its

relation to the ionosphere, and radio astronomy. The work

of the 16 expeditions (including 4 from U.S.A.) in or near

Khartoum on these is then summarized. (Met. Abst. 4. 5-251.)

--C.E.P.B.

311
D-864 Wachtler, Maximillian, Funkpeilunqen des ersten kunstlichen Erdsatelliten Sputnik. (Radio bearing taken from

the first artificial satellite of the earth. Sputnik. ) Deutsche Hydrographische Zeitschrift, Hamburg, 10(5): 169-175.

6 figs. , table, 2 refs. German, English and French summaries p. 169. DWB--Information is given about the radio

bearings taken from the first satellite Sputnik on Oct. 16

and 17, 1957, on a frequency of 20, 005 Mc. A special

feature is that the results obtained by application of the

twin channel visual direction finder are pure line indications. The different series of observations show a variation of the bearings in a clockwise direction as well as

in anti-clockwise direction, covering angles between circ.

4 and 171 . These bearings for a shortwave transmitter

beyond the ionosphere were compared with bearings for two

very distant stations on nearly identical frequencies which

both show the elliptical split being characteristic of coherent waves. (Met. Abst. 12. 7-73. ) -Author's abstract.

D-865 Wait, James R. (Nat'l. Bureau of Standards, Boulder,

Colo. ), The. attenuation vs. frequency characteristics

VLF radio waves. Institute of Radio Engineers, N. Y.

,

Proceedings, 45(6):768-771, June 1957. 10 figs. , 7 foot - refs. , eqs. DLC--The theoretical dependence on frequency

of the attenuation of the wave guide modes in VLF propagation is discussed in some detail. It is indicated that most

of the published experimental data between 1 and 30 kc was

compatible with the sharply bounded model of the ionosphere with a reflecting height of about 70 km during the day

and 90 km during the night. (Met. Abst. 9. 8-158. ) -Author's abstract.

D-866 Wait, J. R. , A survey and bibliography of recent research

in the propagation of VLF radio waves. U.S. National Bureau of Standards, Technical Note, 58, May 1960. Ground

wave propagation, 38 refs. ; Characteristics of the lower

ionosphere, 16 refs. ; General theories for propagation in

inhomogeneous medium, 15 refs. ; Calculations of ionospheric reflection coefficients, 26 refs. ; Measured ionospheric reflection coefficients (VLF), 11 refs. ; Mode

theory of ELF and VLF ionospheric propagation, 51 refs. ; Theory of the propagation of pulses in ELF and VLF ionospheric propagation, 9 refs. ; Characteristics of lightning

discharge, 29 refs. ; Atmospheric wave forms (VLF), 29

refs. ; Atmospheric wave forms (ELF), 18 refs. ; Measured

amplitude characteristics of VLF fields, 18 refs. ; Measured phase characteristics of VLF fields, 18 refs. ; Noise

(ELF), 16 refs. ; Whistlers and magneto-ionic duct propagation, 26 refs. ; Exosphere and Dawn Chorus, 9 refs. --

312
The survey is confined primarily to terrestrial propagation.

Solar and exosph >ric phenomena generally excluded.

D-867 Waldmeier, Max, Ein neuer Effekt chromospharischer

Eruptionen. (A new effect of chromospheric eruptions.

)

Naturwissenschaften, 44(16):439, Aug. 15, 1957. fig.

DWB--An eruption was seen on E limb of sun, 1046-1230

world time, on April 16, 1957. There was total fading

(Mogel-Dellinger effect) on 5320 m and increase on 1950 m.

(Met. Abst. 8. 11-279. )--C. E. P. B.

D-868 Waldmeier, M. (Zurich), Fortschritte der Radioastronomie . (Progress in radio astronomy. ) Naturwissenschaftliche Rundschau, Stuttgart, 12(7): 243-254, July 1959. 9

figs. , 3 tables. DWB, DLC--The progress in radio astronomy, as presented at the symposium of the Astronomical

Union and Radio Union held in Paris, July 30 to Aug. 6,

1958, is reported on under the subjects: moon, planets

and comets, and especially on the sun. The radio emission of the calm sun, the radiation of coronal condensations, of R areas, radiation eruptions, the radio astronomical exploration of the outer corona, and solar terrestrial relations are dealt with. Technical problems are discussed under the following headings: structure of our stellar system, observations on radio sources, their optical

identification, and hydrogen in galactic and extra-galactic

star systems. Photographs of the 25 m radiotelescope of

the Maryland Point Observatory, of the 15 m radiotelescope of the Naval Research Laboratories, Washington,

and of the expanding gas mist shell in Cygnus, taken by

the 25 m Schmidt Refractor at Mt. Palomar, are among the

illustrations. (Met. Abst. 11. 9-105. )--O.T.

D-869 Warren, E. and Muldrew", D. , A method for computing

ionospheric focusing of radio waves, using vertical incidence ionograms. Institute of Radio Engineers, New York,

Transactions, Vol. AP-9(4):403-409, July 1961. 15 figs.

,

14 refs. , 19 eqs. DLC--The dependence of the signal

strength of radio waves upon ionospheric focusing and spatial attenuation is calculated for a spherical ionosphere in

terms of parameters obtainable from the appropriate vertical

incidence ionogram. The signal strength at any given distance can be presented as a function of these ionospheric

parameters in the form of a contour chart from which the

unabsorbed field strength can be obtained easily as a function of frequency. The geometrical optics approximation is

used. The limits of the region at the skip distance for

313
which this method fails are estimated by comparing the re- sults of a ray and a wave type calculation. --Authors' abstract.

D-870 Warwick, Constance (Nat'l. Bur. of Standards, Boulder,

Colo. ) and Warwick, J. W. (High Altitude Obs. , Boulder,

Colo.), Flare associated bursts at 18 Mc/s. (In: Paris

Symposium on Radio Astronomy, July-Aug. 1958, (Proceedings), pub. Stanford Univ. Press, 1959. p. 203-207. 4

figs. , table, 9 refs. DLC--This study is limited to those

bursts closely associated with an SCNA, and with a re- ported flare or SWF. The relation to bursts at other frequencies to associated flares and to geomagnetic disturbances were investigated. It is concluded that while flares or SCNA's with associated 18 Mc/s bursts provide a promising means of forecasting geomagnetic disturbance, they

appear to offer no essential improvement over forecasts

made on the basis of optical flares characteristics and ra- dio noise bursts at higher frequencies. Despite the higher

level in the solar atmosphere at which the 18 Mc/s disturbance occurs, the relation to geomagnetism does not sharpen.

--E. Z. S.

D-871 Warwick, C. and Wood, M. (both, Nat'l. Bur. of Standards, Boulder, Colo. ), A study of limb flares and associated events. Astrophysical Journal, Chicago, 129(3) :801-811,

May 1959. 6 figs. , 4 tables, 14 refs. DWB, DLC -Measured heights of limb flares were used to derive a frequency

distribution of flare height and to assess the importance of

height in the production of flare associated events. The observed height distributions can be explained by a real distribution with maximum at zero, decreasing toward greater

heights. The occurrence of SWF (short wave fadeout) depends strongly on flare height. This dependence could be

explained as an effect either of absorption of the ionizing

radiation in the sun's atmosphere or of a mechanism of production of ionizing radiation that depends critically on the

height of the flare. Center-to-limb variation of SWF occurrence, while not conclusive, favors the former interpretation.

The relation between optical flare characteristics and occur- rence of associated bursts of radio noise is strongest for

decimeter bursts and weaker for bursts at meter wave lengths.

(Met. Abst. 11.5-100. )--Authors' abstract.

D-872 Warwick, James W. , Research carried out June 15-Sept. 15,

1955, (at the High Altitude Observatory) . Colorado Univ.

High Altitude Observatory, Climax, Contract AF 19(604)-

1491, Scientific Report, No. 1, Jan. 10, 1956. 9 p. 8 refs.,

13 eqs. DWB--

314
Pt. IV, p. 6-8, gives the results of the author's solution of

the problem of wave propagation of discrete radio noise

sources in the ionosphere, assuming an accumulation of net

charge in a magnetic field and with oblique incidence of the

wave on a stratified region for normal incident, reflected,

and transmitted waves. This solution was found to have

been worked out previously by K.C. WESTFOLD in Australia

(1949). Notes on the author's visit to the Jodrell Bank Radio

Observatory in connection with the International Astronomy

Conference at Dublin are included. (Met. Abst. 9A-140.

)

--M. R.

D-873 Warwick, J. W. , Current (Sept. 1955) status of English and

French radio astronomy research on ionospheric and atmospheric problems. Colorado. Univ. High Altitude Observatory, Climax, Contract AF 19(604)-1491, Scientific Report,

No. 2, Jan. 8, 1956. 5 p. DWB--A summary of research

under way at Manchester Univ. , Cambridge, London, and

Paris, along the lines of radio star scintillation measurements at VHF range, to determine ionospheric winds, eclipse

results in June 30, 1954 and studies of scattering at 9350

Mc/s based mainly on unpublished work. (Met. Abst. 9A139. )-M. R.

D-874 Warwick, J. W. and Zirin, H. , (Comments on) Chubb. T. A. ; Friedman. H. ; Kreplin. R. W. and Kupperian, J. E. . Jun. : Rocket observation of X-ray emission in a solar flare.

Nature, London, 180(4584) :500-501, Sept. 7, 1957. 8 refs.

Reply by Chubb et al. Ibid., p. 501-502. DWB--On July

20, 1956, during a solar flare which gave normal Lyman

Alpha and enhanced X-ray emissions from the sun, cosmic

noise fell to 93% of average at 1912 U. T. , becoming normal

again by 1920. The origin of 3-A-X-rays is discussed; the

possibility is considered that they are produced locally in

the earth's atmosphere. CHUBB et al. point out that X-rays

were detected only when the photon counter in the rocket

could "see " the sun. The X-ray source increased electron

density in the D layer by 40%. (See ref. D-126 . ) (Met. Abst. 9B-166.)--C.E.P.B.

D-875 Warwick, J. W. and Zirin, H. , Research carried out Oct. 1-

Dec. 31. 1956 (at the High Altitude Observatory) . Colorado.

Univ. High Altitude Observatory/ Climax, Contract AF 19

(604) -1491, Scientific Report, No. 6, April 1, 1957. 6 p.

2 figs. , 9 refs. , 7 eqs. DWB (M10. 535 C719s) -Construction of the 18 Mc/s wide angle interferometer continues

through the report period. The antenna superstructures were

essentially completed, in unassembled form, receiver tests

on Ewen-Knight Radio Astronomy Receiver Model 1620

315
continued, but were not completed during the period. In

view of the incomplete status of the equipment, we decided

to devote time to analysis of the records from the IGY Radio

Flare Detector, constructed at HAO with funds from another

source. The records show the intensity of cosmic noise (at

18 Mc/s ) vertically incident through the ionosphere. We

are able to derive from these records the march of electron

density as a function of time of day and height in the D re- gion. Surprisingly, we also can discuss the variation of

recombination coefficient within a limited height range of

the D region. The electron density curves fit, more or less,

those derived in different ways by other groups. On the

other hand, we predict that the recombination coefficient

either is constant with height (in the D region), or increases

upwards. (Met. Abst. 11F-149.) --Authors' abstract.

D-876 Warwick, J. W. , Radio observations of Soviet satellites,

1957 Alpha 2 and 1957 Beta 1. International Geophysical

Year, 1957/1958. IGY World Data Center A (Rockets and

Satellites), National Academy of Sciences, Wash. , D. C.

,

IGY Satellite Report Series, No. 5, July 30, 1958. 50 p.

26 figs. , table, 47 eqs. Also issued as: Colorado. Univ.

High Altitude Observatory, Boulder, Scientific Report, No.

10, DWB (629. 1388 W299ra)--A report is given on the preliminary results of the analysis of U. S. 20 Mc/s radio observations of Soviet satellites 1957 Go 2 and 1957^ 1, the

problems involved, the cataloguing of various kinds of ionospheric fading, the interferometric effects of these satellites

and the basic fading on the records. Details on the spin-fading characteristics of rotating and circularly polarized an- tenna systems are also discussed and analyzed in full. (Met.

Abst. 11. 1-109. )-N. N.

D-877 Warwick, J. W. , Measures of ionospheric absorption and

refraction at 18 megacycles/second. Colorado. Univ. High

Altitude Observatory, Contract AF 19(604) -1491, Final Report, Dec. 15, 1958. 9 p. 2 figs. , 10 refs. DWB (M10.

535 C719s)- -Ionospheric absorption and refraction at a frequency of 18 Mc/s has been measured by means of the techniques of radio astronomy. A description of the two experiment techniques used is given in this report. (Met. Abst.

11F-150.)-N.N.

D-878 Watts, J. M. (Nat'l. Bur. of Stand. , Boulder, Colo.), Audio- frequency electromagnetic hiss recorded at Boulder in 1956.

Geofisica Pura e Applicata, Rome, 37(169-173, 1957. 4 figs.,

3 refs. DLC --Hissing noise is very frequently heard on re- ceivers used for detecting whistlers during geomagnetic disturbances. This phenomenon may be associated with the

316
"dawn chorus " or whistlers, but is distinct from either and

also from sferics. The energy is concentrated in narrow

band widths that fluctuate, giving a surging rather than a steady hissing effect. Relative amplitude of the hiss, compared with the geomagnetic field records, is shown graphically. The hissing begins about 8 hrs after the rapid commencement of the storm. Records show the peak energy of

the hiss was near 3 kc. Variations in spectra of hiss frequency are illustrated by numerous reproduced records from

March-Dec. 1956, hissing was heard on 9 out of 15 major

magnetic storms recorded at Boulder, Colo. , at Sunset Field

Station. (Met. Abst. 10. 1-134. )--M. R.

D-879 Watts, J. M. (Nat'l. Bureau of Standards, Boulder, Colo. ),

An observation of audio frequency electromagnetic noise dur- ing a period of solar disturbance. Journal of Geophysical

Research, Wash., D.C., 62(2): 199-206, June 1957. 5 figs.,

6 refs. DLC--An unprecedented cosmic ray increase occur- red on Feb. 23, 1956. Recording apparatus for the regular

collection of examples of whistlers began operating at

Boulder, Colo. , on the evening of Feb. 26 — when hissing

noise was being ^ceived. A narrow band receiver tuned to

15 kc showed no response to hiss on Feb. 26 but on March

3 noise was heard. Instead of being a steady hiss, the nar- row band noise oscillated in amplitude, rising and falling

with a period of about 2 sec. This suggested a changing

spectrum in the vicinity of 15 kc. Pictures of the spectra

are shown. Their essential features are: each spectrum

was quite narrow. The center frequency was near 3 kc. The

high frequency side of the peak in energy showed significant

variation from hour to hour. The correlation of hiss amplitude

with magnetic record is shown for March 3-4, 1956. The

strong hiss was followed by only a small enhancement of the

night airglow in the north. The hiss started 8 hrs after the

initial field perturbation, but the fact that it coincided with

the reversed phase may be significant. (Met. Abst. 12. 7-

142.)-E.Z.S.

D-880 Webster, H. C. (Physics Dept. , Univ. Queensland, Brisbane),

A study of "spread F " ionospheric echoes at night at Brisbane,

Pt. 4, Range spreading. Australian Journal of Physics, Melbourne, ll(3):322-337, Sept. 1958. 10 figs. , 8 refs. , 20 eqs.

DLC--In the course of investigations of satellite echoes from

the F region of the ionosphere, it was noted that F and Es

traces recorded at night, on h't equipment at frequencies well

below vertical, are broader than anticipated and tend to change

in a characteristic manner as the gain of the receiver is lowered. In this paper, a quantitative explanation of these phenomena is elaborated, based on the postulate of a "rough"

317
ionosphere. This theory leads to a method whereby, from

the swept -gain h't records, estimates of roughness index

can be formed. These estimates compare satisfactorily, on

a statistical basis, with estimates by other methods. The

theory is extended to the case of multiple hop reflections,

and to the satellite traces; general agreement with experiment is found. Evidence is presented that the ionosphere

appears rougher when transmitter and receiver are adjacent

than when they are widely separated, and a tentative ex- planation is suggested. From the roughness indices, the

relative intensities of Z- and O-mode F echoes for Brisbane

are computed and the rare appearance of Z traces on Brisbane records is satisfactorily explained. (Met. Abst. 11F154. )--Author's abstract.

D-881 Weisbrod, S. (Smyth Res. Assoc. , San Diego, Calif. ) and

Colin, L. (Griff iss AF Base, Rome, N. Y. ), Refraction of

very high frequency radio signals at ionospheric heights.

Nature, London, 184(4680): 119, July 11, 1959. fig. ,2 refs.

DWB--A note and a graphical representation related to the

subject of refractive errors caused by the Earth's atmosphere in the elevation angle determination. It is shown that

in the case of radio tracking of space vehicles, the refractive errors due to the troposphere rapidly decrease with an

increase in the elevation angle, while those due to the ionosphere initially increase with the elevation angle, and then

gradually fall off. (Met. Abst. 11. 11-59. )--I. S.

D-882 Wells, H. W. (Carnegie Inst, of Washington, D. C), Ion- ospheric effects of solar eclipse at sunrise. Sept. 1, 1951 . Journal of Geophysical Research, 57(2):291-304, June 1952.

9 figs. , 6 refs. , 3 eqs. MH-BH--Ionospheric observations

at three stations in Maryland and Virginia during annular

eclipse of Sept. 1, 1951 did not show significant increases

of ion production. They indicate that coronal radiation is

not an important factor in production of F2 ionization. (Met.

Abst. 5. 1-119.)-C.E.P.B.

D-883 Wells, H. W. (Carnegie Inst, of Wash. , Wash. , D. C. ),

F - scatter at Huancayo, Peru, and relation to radio star

scintillations. Journal of Geophysical Research, 59(2):273-

277, June 1954. 2 figs. , 6 refs. MH-BH--The scattering of

radio waves by the F region of the ionosphere at an equatorial location (Huancayo, Peru) was discussed by BOOKER and

WELLS (1938). Subsequent analysis reveals pronouncedly

diurnal, seasonal, and annual characteristics. It is fundamentally a night time event, with greatest frequency of oc- currence in the period from four hours before midnight to

318
four hours after midnight. The scattering is most prevalent

during seasons when the sun is overhead and is infrequently observed during May, June, July, and August (local

winter) when the noon solar zenith angle becomes as great

as 35 . The relative total annual occurrence of F region

scatter for the period 1938 through 1945 shows low values

during 1941-1942, followed by a rapid increase through

1946, which is not closely related to solar activity. The

diurnal properties of F scatter closely correspond to re- ported characteristics of radio star scintillations with peak

activity around midnight. However, the annual or seasonal

properties are not in simple agreement. (Met. Abst. 6D270. )--Author's abstract.

D-884 Westerhout, Gart, Het Radioastronomische Symposium in

Jodrell Bank. (Radio Astronomy Symposium at Jodrell Bank.)

Hemel en Dampkring, The Hague, 54(1):4-13, Jan. 1956.

DWB, DLC--An account of the results of astronomic research

carried out with radiotelescopes: studies on the 21 cm line,

in the vicinity of Orion, heavy water in the universe and absorption of radio sources by hydrogen clouds. The supernova Cassiopeia A, the possible existence of a radio galactic system, and the limit of the universe are summarized.

Photographs of radiotelescope installations, of hydrogen

clouds around the Orion association, of the first radio

astronomy star map, etc. , are included. (Met. Abst. 8. 11-

39.)-I.L.D.

D-885 Westerhout, G. , The radio galaxy. Scientific American,

N.Y. , 201(2):44-51, Aug. 1959. figs. DLC, DWB--Radio

astronomical observations show the spiral structure of our galaxy, with outward surging waves of hydrogen. The spiral arms of the nebula have their origin near the center of

the Milky Way in the constellation Sagittarius. Interstellar clouds of dust obscure this spiral structure from visual

telescopes but not from radio telescopes. Much of the fine

structure of the galaxy has been observed and mapped on

21 cm wave length at the Leiden Observatory's 82 ft radio

telescope at Dwingelov. Different wave lengths show up

different features on radio maps. Details of telescope and

records, and explanation of thermal and nonthermal radiation are presented in this article and illustrated. Origin

of new stars is also explained from new data. (Met. Abst.

11.8-74.)-M.R.

319
D-886 Westfall, W. D. (U. S. Navy Electronics Lab. , San Diego,

Calif.), Prediction of VLF diurnal phase changes and solar

flare effects. Journal of Geophysical Research, Wash., D.

C, 66(9): 2733-2736, Sept. 1961. fig., 2 tables, 6 refs.

,

10 eqs. DLC--VLF diurnal phase shift data are compared

with predictions resulting from the wave guide equations

for the first order mode. The effects of higher order mode

energies appear to exist out to 2700 km, and may at times

affect measurements beyond this range. A relation is given

for the prediction of diurnal phase shift for 10-20 kc radio

waves. Expressions are given for relating observed VLF

phase perturbations caused by both small and large solar

flares to the resulting apparent decreases in ionospheric

reflecting height. (Met. Abst. unpub. ) --Author's abstract.

D-887 Wexler, Raymond (Allied Res. Assoc. , Inc. ), Satellite

observations of infrared radiation. U. S. Air Force. Cambridge Research Center, GRD Research Notes, No. 36:

153-180, June 1960. 13 figs. , 3 tables, 13 eqs. DWB--

A discussion of the proposed meteorological satellites

carrying several infrared sensing elements intended to provide information on the infrared properties of the atmosphere. From available experimental data on absorptions

by atmospheric gases, atmospheric transmissions in the

infrared have been determined. The actual amounts of

radiation which may be expected to leave the top of the

atmosphere over the U. S. on a specific occasion (March

6, 1959, 000Z) are mapped for the "window" regions, the

6. 3/o H«0, the 15 fie , the 4. Z fio C02 and ozone bands.

For the H«0 band, computations are made at air masses

(secant of the zenith angle) for zenith angles of , 60

and 81. 5°. (Met. Abst. 11J-194. )--I. S.

D-888 Whale, H. A. (Seagrove Radio Res. Station, New Zealand),

The effects of ionospheric irregularities and the auroral

zone on the bearings of short wave radio signals. Journal

of Atmospheric and Terrestrial Physics, London, 13(3/4):

258-270, Feb. 1959. 8 figs. , 12 refs. , 5 eqs. DLC--The

nature of the observed variations in the received bearing of

the signals from short wave radio stations at various distances is discussed and the origins of some of the effects are suggested. The major part of the daily variation of

bearing of stations up to about 15, 000 km distant arises

from the refraction of the ray in the Fl region when it is

reflected from the F2 region. A discussion of the curving

of the ray path by successive small changes of direction

at each reflection point leads to the concept of an antipodal

320
area replacing the geometrical antipodal point. The large

changes in direction associated with the passage of a ray

through the auroral regions suggest a method of plotting

the shape of the absorbing parts of the auroral zone by observations at a place remote from this zone. A sample

plot obtained by this method is presented. (Met. Abst.

12. 4-357. ) --Author's abstract.

D-889 Wheelon, A. D. (Space Technology Labs. , Inc. , Los

Angeles, Calif. ) f Relation of turbulence theory to ionos- pheric scatter propagation experiments (summary only).

Journal of Geophysical Research, Wash., D. C. , 64(12):

2230-2231, Dec. 1959. ref. , eq. DLC-The subjects discussed are: 1) statistical behavior of ionospheric scatter

signals; 2) scattering of electromagnetic waves by turbulent irregularities; 3) spectrum of electron density deviations and its relation to turbulence; 4) signal level and

scattering heights, and finally, 5) an explanation is given

of some SID features in terms of increased attenuation.

(Met. Abst. 11E-168.)--W.N.

D-890 Whipple, Fred L. and Davis, Robert J. (both, Smithsonian

Astrophysical Obs. , Cambridge, Mass. ), Proposed stellar

and interstellar survey. Astronomical Journal, New Haven,

Conn. , 65(5): 285-290, June 1960. 6 figs. , 15 refs. DLC--

Previous planning for the design, construction and operation

of an astronomical telescope in a satellite orbit was presented by members of the Smithsonian Astrophysical and Harvard

College Observatories (R. J. DAVIS, R. E. MC CROSKY,

F.L.WHIPPLE and C.A.WHITNEY, Astron. J. 64, 50, 1959).

Further elaboration of these plans is presented, including

possible systems for measuring bright line radiation of the

interstellar medium and obtaining slitless spectra of stars,

as well as a broad survey of the entire sky in three colors

between 1000 and 3000 A. With the support of the National

Aeronautics and Space Administration the design program is

under way at the Smithsonian Astrophysical Observatory.

Plans are also developing for an Aerobee rocket firing in

late 1960 or early 1961 in which a TV image tube system

covered by a multicolor mosaic filter can produce a preliminary shallow survey of both nebulosity and bright stars

over a strip of the sky some 150 by 4 . Since the rocket

will be neither precisely stabilized nor controlled at high

altitudes, the exact position of the observational strip can

only be approximated. Direct image photographs of stars

and nebulosity, however, will be available in spectral re- gions from below Lyman-alpha to approximately 2000 A.

The Westinghouse Electric Corporation has under-taken the

321
development of special materials for TV image tubes sensitive to spectral regions in the far UV. The precise spectral

regions in which the rocket and satellite experiments will

be conducted depend upon these developments. The astrophysical significance is discussed of the proposed experiments in the regions of Lyman-alpha and above for stars

and interstellar material. (Met. Abst. 1 1L -30. )- -Authors'

abstract.

D-891 Whitehead, J. D. , The absorption of short radio waves in

the D. E, and F regions of the ionosphere. Journal of Atmospheric and Terrestrial Physics, N. Y. , 16(3/4): 283-290,

Nov. 1959. 6 figs. , 16 refs. DWB, DLC--The published

values of the noon absorption of radio waves of frequencies 2, 2-4, 4 and 4- 8 Mc/s measured at Slough from 1947

to 1953 have been analyzed. From the absorptions of 2 and

2 '4 Mc/s waves, it has been deduced that (a) the electronic collision frequency 1/ , at the height of the maximum

electron density in the E region when the sun's rays are incident vertically on the ionosphere, is (1. 9 + 0. 1) x 102* per sec; and (b) the normal absorption in the D region increases with increasing sunspot number, whereas the additional absorption which occurs on certain winter days and

arises in the D region may decrease with increasing sun- spot number. The 4 and 4. 8 Mc/s waves were reflected

from the F region at noon. The absorption in the F region

is calculated from the known total absorption and the calculated absorption in the D and F regions. The collision frequency in the F region may then be found. At the height of

reflection of 4 Mc/s waves (150 to 180 km) it is (3. 6 + 0. 6)

X 103 per sec, and at the height of reflection of 4.8 Mc/s

waves (180 to 200 km) it is (3. + 0. 6) X 103 per sec. The

significance of these results is discussed. (Met. Abst.

11F-157.) -Author's abstract.

D-892 Whitehurst, R.N. ; Mitchell, F.H. and Copeland, J.,

Solar radiation and atmospheric attenuation measurements

in the 7 to 8 mm wavelength range. American Physical

Society, Bulletin, 1(5):265, June 21, 1956. -Application

of Dicke radiometer constructed by the authors. --CSIRO

abstract.

D-893 Whitehurst, R.N. and Mitchell, F.H. (both, Univ. of

Alabama, Univ. , Ala. ), Solar temperature and atmospheric

attenuation in the 7-8 mm wavelength range. Institute of

Radio Engineers, N.Y., Proceedings, 44(12): 1879- 1880,

Dec. 1956. fig. , 6 refs. DLC--A record showing results

of a transit of sun through antenna beam of a 7. 5 mm

322
radiometer lasting about 14 min indicates antenna temperature of 720 K when sun is in beam. This and other tests

give sun temperature - 6000 + 500 K, and values of vertical attenuation of 0. 3 to 0. 6 db for weather ranging from

clear to overcast with moderate rain. Solar temperatures

are in keeping with those expected, but attenuation in

cloudy and rainy weather is somewhat smaller than anticipated. A Dicke type radiometer, and 18 in. paraboloidal

antenna were used. (Met. Abst. 11. 5-163. )--M. R.

D-894 Whitfield, G. R. and Hogbom, J. (both, Mullard Radio

Astronomy Obs. , Cambridge, Eng. ), Radio observations

of the comet Arend-Roland. (In: Paris Symposium on Radio

Astronomy, July-Aug. 1958, (Proceedings), pub. Stanford

Univ. Press, 1959. p. 56-57. table, 2 refs. ) DLC (QB475.

P26)--A note on the observations made at Cambridge, England, between March 12 and May 13, 1957 of the comet

Arend-Roland. The observations were made with five different instruments including two interferometers of large

resolving power. The possibility of radio emission from

the extended tail was investigated by observing radio stars

through it. No detectable effect was observed. The upper

limits of the flux density are presented in tabular form.--

I.S.

D-895 Whitney, H. ; Strick, H. ; Aarons, J. et al. (all, A. F.

Camb. Res. Lab. , Bedford, Mass.), Sudden amplitude

variations of Sputnik III signals. Journal of Geophysical

Research, Wash. , D. C. , 65(12):4210-4212, Dec. 1960.

3 figs. , ref. DLC --Amplitude recordings of the 20 Mc/s

signals from Sputnik III (1958 Delta II) were made at the

Sagamore Hill Radio Observatory in Massachusetts. An

interesting feature of the recordings was the presence of

"dropouts ", i. e. sudden decrease of the signal either to

noise level or close to noise level. Two different types

of events responsible for these dropouts are postulated.

One event is wide in geographical extent and the other is a localized effect which is frequency dependent. The

dropout was due mainly to changing transmitter characteristics resulting in reduced power output. The cause of the

changing characteristics was that the satellite had entered

a region of high electron flux. In the instances in which

dropout was observed at some locations or frequencies and

not at others, the reduced signal was due to the intervening medium rather than to the transmitter itself. The two

causes are best differentiated by taking simultaneous observations at several geographical positions. --E. Z. S.

323
D-896 Wild, J. P. and McCready, L. L. , Observations of the

spectrum of high intensity solar radiation at metre wavelengths. I. The apparatus and spectral types of solar

burst observed. Australian Journal of Scientific Research,

Ser. A, Physical Sciences, 3(3):387-398, Sept. 1950. 3

figs., 2 plates (one fold.), table, 7 refs. , 6 eqs., append.

DWB--The authors describe the apparatus and method for re- cording the spectrum of the high intensity radio frequency

radiation emitted by the sun in the frequency range 70 - 130

Mc/s. Results indicating the different kinds of spectra in

solar bursts and the relationship of these bursts to those

observed by means of single frequency equipment are discussed. A special discussion on the effective area and

design of the rhombic aerial, which is used to receive the

radiation, is appended. (Met. Abst. 2. 8-82. )--I.L.D.

D-897 Wild, J. P. , Observations of the spectrum of high intensity solar radiation at metre wavelengths. II. Outbursts.

Australian Journal of Scientific Research, Ser. A, Physical Sciences, 3(3):399-408, Sept. 1950. 2 figs. , 2 fold,

plates, 2 tables, 18 refs. , eqs. DWB--The author describes observations of the spectrum of solar radio frequency radiation in the frequency range 70-130 Mc/s. The

apparatus and method of recording the spectrum is described in article by WILD and MC CREADY. The correlation

of outbursts and other solar radio frequency emissions

with solar flares and magnetic storm is discussed. The

spectra are interpreted as the result of "surge " prominences in the solar atmosphere and the factor causing the

surge phenomenon corresponds to the particles that bring

about terrestrial magnetic storms. (Met. Abst. 2. 8-83. ) --I.L.D.

D-898 Wild, J. P. , Observations of the spectrum of high intensity solar radiation at metre wavelengths. HI. Isolated

bursts. Australian Journal of Scientific Research, Ser. A,

Physical Sciences, 3(4):541-557, Dec. 1950. 7 figs. , 4

plates, table, 12 refs. , eqs. DLC- -Elaborate colored

graphs show the time-intensity relationships of solar radiation "bursts " of various frequencies between 70 and 130

Mc/s in support of article which gives a thorough analysis

of observations made at Sydney, Australia, during June

1949. Thirty-two isolated bursts were recorded in 264 hrs

of observation and 3 types of bursts defined; energy spectra are given for 4 isolated bursts, and a good correlation

shown between frequency and energy distribution. (Met.

Abst. 3.9-127.)-M.R.

324
D-899 Wild, J. P. , Observations of the spectrum of high intensity

solar radiation at metre wavelengths. IV. Enhanced radiation. Australian Journal of Scientific Research, Ser. A,

Physical Sciences, 4(l):36-50, March 1951. 9 figs. , plate,

refs. DLC--In this final paper of a series, author refers to

the theoretical work by other scientists and after briefly summarizing their work gives a detailed analysis of the high intensity solar radiation at 70-130 Mc/s. The results indicate

that "storm bursts" (i. e. , short lived narrow band bursts)

have defined properties and suggest a possible new approach

to the theoretical problem of the "enhanced radiation." (Met.

Abst. 5. 6-133.)--W.N.

D-900 Wild, J. P. and Roberts, J. A. , Regions of the ionosphere

responsible for radio star scintillation. Nature, London,

178(4529) :377-378, Aug. 18, 1956. fig. , 3 tables, 6 refs.

DWB--Observations of scintillations of radio source in Cygnus A at 15 elevation from Dapto, N. S. Wales, 1952-55,

showed nighttime correlation with spread F and daytime with

sporadic E. Fluctuations were greatest at midnight in midwinter and noon in mid summer. At night only there is a WE component of motion of 80 m/s across the ground, which

is attributed to the effect of the earth's rotation on stationary irregularities at 500 km. (Met. Abst. 8.2-298.)--

C. E. P. B.

D-901 Wild, J. P. and Roberts, J. A. , The spectrum of radio star

scintillations and the nature of irregularities in the ionosphere. Journal of Atmospheric and Terrestrial Physics,

8(l/2):55-75, Feb. 1956. 17 figs. , table, 15 refs. DWBObservations were made at Sydney, Australia, on the radio

source in Cygnus, of intensity at one point as a function of

time and frequency (40-70 Mc/s), the phase gradient as a function of time, and the intensity at 45 Mc/s at corners of a triangle. Instrumental set-up is described and specimen

records shown and discussed. The spectra suggest that most

of the irregularities are due to focusing by single lenslike ir- regularities. The scale size of structures causing spectral

patterns is above 3 km. In some cases random effects predominate, due to finer structure. Degree of fluctuation

shows maxima near midnight (winter) and midday (summer).

In many cases the pattern on the ground is very elongated

(3 or 4 to 1). Apparent motion was mainly W - E, 80 m/s,

in winter, variable in summer. (Met. Abst. 7.8-116.)-- C E. P. B.

325
D-902 Wild, J. P. (Div. of Radiophysics, C. S. I. R.O. , Sydney)

and Zirin, H. (High Altitude Obs. , Univ. of Colorado,

Boulder ) , On the association of solar radio emission and

solar prominences. Australian Journal of Physics, Melbourne, 9(3):315-323, Sept. 1956. 6 figs. , 6 refs. DLC--

Prominence cinematograms made at Sacramento Peak and

Climax in the years 1949-55 have been examined and compared with the solar radio records at 167 Mc/s. No close

connection was found between limb events and radio events,

but some eruptions were found to be associated with simultaneous radio bursts. Three such cases are discussed in

detail. The limb passages of large sunspots in 1949-55

were studied on both cinematograms and single exposure

surveys with the view of finding a criterion for radio-noisy

spots. It was found that spot groups showing looped prominences and downward streaming from the corona showed a marked tendency to produce radio noise storms. This result

is ascribed to the fact that the seat of such storms must lie

in the corona and in the presence of strong ordered magnetic

fields. (Met. Abst. 9A- 141. )--Authors' abstract.

D-903 Wild, J. P. (Radiophysics Div. , C. S. I. R. O. , Sydney),

Solar radio noise and the study of corpuscular streams from

the sun. (In: Solar eclipses and the ionosphere: a symposium. . . ed. by W. J. G. Beynon and G. M. Brown. London,

Pergamon, 1956. p. 258-260. 2 figs. , 2 refs. ) DWB--

Observations in Australia over several years with a dynamic

spectroscope covering the frequency range 40 - 240 Mc/s

have shown that most sporadic bursts of radio emission from

the sun fall into two distinct spectral classes, having quite

discrete ranges of outward radial velocity. Both types of

radio burst may occur at the time of solar flares. It is

thought that the slower velocities may be associated with

the outrush from the sun of geomagnetic storm particles,

while the very fast range of velocities may be associated

with the ejection from the sun of the agency responsible

for the increase in cosmic rays sometimes observed about

one hour after flares. (Met. Abst. 9A-142. )--Author's

abstract.

D-904 Wild, J. P. and Sheridan, K.V., A swept frequency interferometer for the study of high intensity solar radiation at

meter wavelengths . Institute of Radio Engineers, N. Y. , Proceedings, 46(1): 160-171, Jan. 1958. 15 figs. , 16 refs.,

15 eqs. DLC—The instrument described and discussed is

capable of measuring the one dimensional position and

angular size of a transient source on the sun's disk, determines the polarization and intensity of the received

326
radiation as a function of frequency 40-70 Mc/s. The two

antennas of the main interferometer are spaced at a 1 km

east-west line. The two antennas of the polarization system are erected on a common axis maintained in the direction of the sun. Some preliminary observations have given

an indication of the spectrum of source size for activity of

spectral types I and III. In both cases the angular size is

found to decrease from about 10 min of arc at 45 Mc to

about 6 min of arc at 65 Mc. (Met. Abst. unpub. )- -Authors' abstract.

D-905 Wild, J. P. ; Sheridan, K. V. (both, C. S. I. R. O. , Univ.

Grounds) and Neylan, A. A. (Mt; Stromlo Obs. , Canberra),

An investigation of the speed of the solar disturbances re- sponsible for type HI radio bursts. Australian Journal of

Physics, Melbourne, 12(4): 369-398, Dec. 1959. 16 figs.

,

18 refs. , 11 eqs. DLC--The paper describes an investigation aimed at finding out whether solar radio bursts of spectral type III are due to disturbances which travel out through

the corona with velocities exceeding 0. 1 c, as predicted by

the well known hypothesis that the emissions are due to

plasma oscillations. If the proposition is correct, emissions at different frequencies would be generated at different levels in the corona — the lower the frequency the higher the source. This property is tested by simultaneous directional observations at a number of frequencies between

40 and 70 Mc/s, using a swept frequency interferometer.

The system and performance of the interferometer are described and errors in position finding due to ionospheric re- fraction are discussed. Results for type III bursts show

that different frequencies are generated at different levels

in the corona according to the predicted sequence; they

therefore strongly support the plasma hypothesis. It is concluded that the corona is considerably denser in the regions

where type III sources are generated than in the average

corona as depicted by conventional models; and an origin in

coronal streamers is suggested. The derived velocities of

type III disturbances are found to be considerably greater

than those previously deduced from spectral data alone. The

range of velocities now inferred extends from 0. 2 c to 0. 8 c, with an average of 0.45 c. The significance of these very

high velocities is discussed. For this purpose new evidence

is discussed relating to the "type V" continuum emission

which follows certain type III events. The combined type III- V events, which are known to correlate closely with chromospheric flares and sub-flares, are interpreted in terms of

streams of relativistic electrons with energies /£ MeV which

travel along magnetic lines of force in spiral paths. It is

327
suggested that, in its outward passage, such a stream ex- cites plasma oscillations in the surrounding coronal gas

(yielding the type III burst), while, under favorable circumstances, the electrons themselves emit synchrotron radiation (yielding the type V burst). A possible connection between the energetic solar electrons and the corpuscular ra- diation surrounding the Earth is suggested. (Met. Abst.

11. 12-62. )- -Authors' abstract.

D-906 Williams, W. E. , Jr. , Space telemetry systems. Institute

of Radio Engineers, N. Y. , Proceedings, 48(4): 685-690,

April 1960. table, 14 refs. DLC--This paper presents some

of the problems which are faced in the field of space telemetry, and gives a few examples of the approaches used in attempts to solve these problems to date. The different types

of information to be transmitted back to receiving stations

on the earth from satellites and space probes are discussed.

The telemetry systems (FM/FM, FM/AM, PCM/PM, etc.)

which have been used in various experiments of this type

are described, along with some typical performance figures

for some past payloads. The paper is concluded with a discussion of the problems to be faced in future experiments.

(Met. Abst. 11. 12-486.) -Author's abstract.

D-907 Wilson, Raymond H. , Jr. (Goddard Space Flight Cent.

,

NASA, Wash. , D. C. ), Geomagnetic rotational retardation

of satellite 1959 061 (Vanguard II). Science, Wash. , D. C,

131(3395): 223-225, Jan. 22, 1960. fig. , 9 eqs. , 9 refs.

DLC --Radio observations made during the battery life of

Vanguard II showed that the satellite's rotation was being

retarded exponentially at a rapid rate. Precise analysis of

electromagnetic couples on the conducting and magnetic

parts of the satellite indicates a mean ambient geomagnetic

field of 0. 158 gauss, and confirms the eddy current theory

previously applied to Vanguard I. (Met. Abst. 11. 12-553. ) --Author's abstract.

D-908 Wilson, D. McL. A. (Cavendish Lab. , Cambridge), Electron

density measurements in the upper ionosphere using the

Faraday rotation of radio signals from artificial satellites . Nature, London, 186(4725):623-624, May 21, 1960. fig.

,

2 refs. DWB--Several observers using the Faraday rotation

of radio signals assumed that the ionosphere is spherically

stratified. The signals of satellites 1957 h 2 and 1958 fc 2,

observed at Cambridge, have shown that the variation of the

ionosphere with latitude and longitude must be taken into ac- count near or below the peak of the F2 layer if results consistent with vertical incidence soundings are to be obtained.

328
The effect of the horizontal variation of the ionosphere

is shown. On this occasion the satellite was slightly

above the F2 layer peak. Satellite passes above the F2

peak indicate that the electron density falls off with a scale height of approximately 230 km and the average

ratio of the total electron content above the peak to that

below is 3.4 to 1. (Met. Abst. 11. 12-378. )--E. K.

D-909 Witunski, Michael (McDonnell Aircraft Corp. , St. Louis,

Mo. ), The system design of orbiting astrophysical

laboratories: a report. Societe Royale des Sciences de

Liege, Memoires in 8 , 5th Ser. , 4:60-35, 1961. DLC--

A review of the design and construction of the Orbiting

Astrophysical Laboratory is presented. The advantages

of observations outside the terrestrial atmosphere are emphasized. The apertures of telescopes of 12 in. for

stellar and 3 in. for solar observations will yield results

unobtainable from most powerful ground instruments. In

solar research the problem consists of obtaining a complete trace of the solar spectrum from the x-ray region to

3000 A with as high a spectral resolution as can be obtained. Telescope guidance and attitude control are discussed in relation to perturbation torques. The latter

depend critically on the configuration design of the or- biting satellite, on the earth's magnetic field, the sun's

radiation pressure, air drag and the earth's gravitational

field. The control system may be achieved by several

methods; among them, by the motion of a fly wheel or by gas pressure jets. The guidance system is envisaged

by setting three telescopes on three north pole stars and

three telescopes on three south pole stars. Various

methods for obtaining observational accuracy and the

dynamic interaction of all the systems in the control loop

are discussed. The reliability of various satellite parts

for a year's operation was tabulated. Transmission of

information from the orbiting telescope to the ground stations and the reception, processing and recording of

telemetered data on the stations are outlined. --S. N.

D-910 Wong, Ming S. (AFCRC Propagation Lab. , Bedford, Mass.),

Refraction anomalies in airborne propagation. Institute of

Radio Engineers, Proceedings, 43(9): 1628-1638, Sept. 1958.

16 figs. , foot-refs. , 5 eqs. DLC --Propagation at 250-10,000

mc often encounters dense fadings, radio holes, antiholes or

329
radio ducting. These anomalies are portrayed by ray tracings using a differential analyzer which solves the simplified ray equation

d

2 h

^

n(h. x) + _1_

, 2 h a dx

Both hypothetical-prototype and complex measured refractive index profiles of the atmosphere are used for the ana- log computation of the ray tracings which are interpreted

to explain refraction anomalies in radio wave propagation,

and are compared with signal strength measurements. They

involve divergence of rays, and concentration and crossing

of direct rays in multipath transmission. Resulting radar

angular and range errors of arrival of interfering rays at the

points where they cross, corroborating radio astronomical

data on angular deviation of stars. (Met*. Abst. 10. 5-218. ) --From author's abstract.

D-911 Woodward, R.H. , A tentative model of the sun. Journal

of Geophysical Research, 54(4): 38 7 -396, Dec. 1949. 30

refs. DWB--A theory of the circulation of ions in the

earth's electric field is used as an analogy for the solar

electric field, Sunspots, chromosphere, prominences and

flocculi and corona are briefly described with references

to the ionosphere, solar radio noise and cosmic rays. (Met.

Abst. 2. 5-50.)-C.E.P.B.

D-912 Wright, R. W. ; Koster, J. R. and Skinner, N. J. , Spread F- layer echoes and radio star scintillation . Journal of Atmospheric and Terrestrial Physics, London, 8(4/5): 240-246,

May 1956. 4 figs. , 10 refs. DWB--Observations of radio

star scintillation at Achimota and spread F layer scatter at

Ibadan, both in Gold Coast, 510 km apart, showed an aver- age correlation of 0.46 for 165 pairs. Diurnal and seasonal

variations of spread F layers are plotted. These depend to

some extent on the degree of magnetic disturbance; at Ibadan in winter the scatter on disturbed days is only a quarter

that on quiet days. (Met. Abst. 7. 10-308. )--C. E. P. B.

D-913 Yaplee, B. S. ; Bruton, R.H. ; Craig, K.J. and Roman, N. G.,

Radar echoes from the moon at a wavelength of 10 cm. Institute of Radio Engineers, N. Y. , Proceedings, 46(1): 293-297,

Jan. 1958. 8 figs. , 14 refs. DLC --Radar contact has been

made with the moon with short pulses at 2860 Mc, beginning

a program of short pulse lunar radar. The principal objective

of the program is to obtain more accurate moon-to-earth distances than presently are known. Other information may

330
result from the program, such as the earth's diameter, the

interplanetary electron density, and the lunar surface characteristics. To date, the program has yielded the following

results: earth-moon distances have been measured over

several days with consistencies of less than one-half mile;

several rough reflectivity measurements have been made

which indicate that the radar cross section of the moon is

975 miles at 2860 Mc with pulses of 2^sec duration, and

the fine structure of echoes may be correlated with lunar

topography. (Met. Abst. unpub. )- -Authors' abstract.

D-914 Yee, James S. (Boeing Co. , Seattle, Wash. ), Mutual coupling of two thin infinitely long slots located on a perfectly

conducting; plane in the presence of a uniform plasma layer.

Institute of Radio Engineers, N. Y. , Proceedings, 49(12):

1837-1845, Dec. 1961. 10 figs. , 15 refs. , 82 eqs. DLC--

The investigation of antenna coupling was motivated by a study of communication with a hypersonic vehicle which upon re-entry, introduces a plasma sheath over the antennas.

The model chosen for analysis consists of two infinitely

long thin slots on a ground plane covered by a uniform plasma layer which is assumed to be a lossless gaseous dielectric slab having a dielectric constant less than unity but

greater than zero. The coupling effects are described in

terms of a mutual admittance parameter in an equivalent IT

network from which other admittance parameters are derivable. The problem is formulated by spatial Fourier transforms which, upon inversion, would yield the desired re- sults. The transform integral for the case of a thick plasma

layer is evaluated approximately by the method of steepest

descent. The results are explained in terms of multiple re- flections of rays by the sharply defined plasma-air interface. When the quantities are plotted as functions of slot

separation, the perturbations show up in the form of ripples

about the curve for the unbounded plasma. In a realistic

situation there is no well defined boundary and the rippling

may show up in a statistical manner. The coupling effect

is found to be less serious in the presence of a plasma than

in its absence. When the operating frequency is appreciably higher than the plasma frequency, the change in driving

point admittance is small. Also, inside a thick plasma layer, no unattenuating pole waves are excited. (Met. Abst.

unpub. ) --Author's abstract.

D-915 Yeh, K.C. and Swenson, G. W. , Jr. (both, Univ. of Illinois,

Urbana, 111. ), The scintillation of radio signals from satel - lites . Journal of Geophysical Research, Wash. , D. C. , 64(12):2281-2286, Dec. 1959. 6 figs. , 8 refs. DLC--

331
Signals from satellites 1957 a 2 and 1958 0C2, recorded

during a 20 month period, are analyzed to determine the

diurnal and seasonal variations of the incidence of scintillation. Marked diurnal effects are noted, scintillation being much more frequent at night. Night time scintillation

correlates with the occurrence of ionospheric 'spread F' and

apparently originates in inhomogeneities at heights of about

220 km and, in most cases, at latitudes greater than 40 N.

Daytime scintillation appears to originate in smaller, inhomogeneous regions below 220 km and more widely distributed in latitude. (Met. Abst. 11F-159. )- -Authors' abstract.

D-916 Yeh, L.P. , Communication in space. Electronic Industry

and Teletechnique, 18(3):94-99, March 1959. 9 figs. , 9

tables, 16 refs. DLC --Experimental data obtained from

moon echo experiments and from satellite observations are analyzed and it is concluded that a fading margin of 20 db

should be allowed for in a communication system. Problems

associated with radio transmission and reception in space,

and between satellites and the earth are examined. --IRE Abstract.

D-917 Zachary, W. W. ; Wolff, E. A. and Katzin, M. , Determination of ionosphere parameters by means of a satellite antenna type probe. Electromagnetic Research Corporation, Wash,

D.C., Contract AF 19(604) -6656, Scientific Report No. 1,

June 30, 1960. 52 p. 9 figs. , 11 refs. , 65 eqs. --A spherical antenna type probe for determining the parameters of the

ionosphere is described. This consists of a main slot around

which are disposed pairs of small orthogonal slots. By applying a driving voltage to the main slot and measuring the input

impedance, as well as the voltages induced in the orthogonal

slots, the ionization density, collision frequency, and vector

earth's magnetic field may be determined. These are local

values since the reaction of the medium on the probe is effectively limited to distances of the order of less than a wavelength. As a preliminary to the main analysis, the input admittance of a slotted plane antenna in a magneto-ionic medium

is analyzed. The solution is obtained in a form suitable for

numerical evaluation. Measurement systems for the determination of the quantities necessary to evaluate the parameters of the ionized medium are considered. Three systems

are shown and their relative advantages and disadvantages

are outlined. A suitable measurement system appears to be

quite feasible of realization. (Met. Abst. 11.12-379.)--

Physics Abstracts.

332
D-918 Zelinskaia, M. R. ; Troitskii, V. S. and Fedoseev, L.I.

(all, Gor'kii Univ. ), Lunar radio emissions at 1. 63 cm

wavelength. Soviet Astronomy AJ, N. Y. , 3(4):628-632f Jan. /Feb. 1960. 2 figs. , 13 refs. , 9 eqs. DLC. Transl.

of Radioizluchenie Luny na volne 1. 63 cm, Astronomicheskii Zhurnal, Moscow, 36(4):643-647, July/Aug. 1959.

DLC--Measurements were taken of the temperature of radio

emissions from the central portion of the lunar disc, at

1, 63 cm wavelength, as a function of lunar phase. The

relationship displayed a sufficiently good approximation

to the expression Tn

= 224 - 36° cos {£1 1 - 40°). The

-1

value of the attenuation coefficient l< = 0. 2 cm of the

electromagnetic wave, and the value of the equivalent

conductivity cr - 7. 9 • 1(>3 CGSE of lunar rock, were derived from a comparison with the theoretical relationship.

(Met. Abst. 11L-103. )- -Authors' abstract.

D-919 Zevakina, R. A. , Bukhtoobraznye vozmushcheniia geomac?-

nitnoqo polia i sviazannye s nimi izemeneiia v ionosfere

po nabliudeniiam v Murmanske. (Bay-like disturbances of

the geomagnetic field and associated changes in the ionosphere according to observations in Murmansk. ) Akademiia

Nauk SSSR, Izvestiia, Ser. Geofiz. , No. 2:304-310, Feb.

1959. 4 figs. (incl. photos), 4 tables, 13 refs. DLC--

Bays possess a fully definite diurnal variation. In 1954-

1956 positive bays were observed chiefly in the second

half of the day - negative in the first. The latter are most

frequently observed in summer; the former in winter. Currents producing bay-like disturbances in Murmansk alter

their direction about 20. 00 h. Up to 20. 00 h the current

flows from west to east producing positive bays but from

20. 00 h it flows from east to west and produces negative

bays. 'The center of the currents " in most cases (86%) is

in northern Murmansk. With increase in solar activity the

center of currents is displaced to the south. The majority

of bay shaped disturbances was accompanied by anomalous

variations in the ionosphere. Most frequently (more than

50%) the bays were accompanied by an increase of the limiting frequencies of Es layer. About 25% of the bays are accompanied by complete absorption of radio waves. With

increase of magnetic activity the character of ionospheric

variations associated with bay shaped disturbances varies

somewhat and the frequency of anomalous variations in the

F2 region increases. The appearance of sporadic "Es clouds

with high limiting frequencies and complete absorption over

Murmansk during bay shaped disturbances indicates the

penetration of corpuscular currents overhead. At the same

time the center of the source of bay shaped disturbance in

most cases is north of Murmansk. (Met. Abst. 11. 8-105.

)

-I.L.D.

333
D-920 Zhekulin, L. A. , Raspredelenie elektronnoi kontsentratsii

s vvsotoi po dannym opytov s raketami i iskusstvennvmi

sputnikami Zemli i ee vliianie na rasprostranenie radiovoln. (Distribution of electron density with height according to

data from rocket and artificial satellite experiments and its

effect on radio wave propagation. ) Iskusstvennye Sputniki

Zemli, Moscow, No. 1:67-79, 1958. 5 figs. , 7 refs. , 27

eqs. DLC--With the aid of relevant equations, the author

presents a comprehensive examination of the propagation

of radio waves at high altitudes. The contents of this paper

include the following, viz: distribution of the density of

ionization with height; effect of the distribution of ionization, as disclosed by the most recent experiments, upon the

propagation of radio waves; extinction of radio waves; and

unstable processes in the reflection of an electromagnetic

signal from a non-homogeneously ionized layer. The solution of the problem of the propagation of electromagnetic

waves in the ionosphere with the distribution of ionization

is expressed in Airy functions. A sharp variation of the

ionization gradient occurs in the E layer of the ionosphere

since the continuous and approximately monotonic increase

of ionization with height is maintained. Hence, with increase in the frequency, the level of reflection of electromagnetic waves is displaced gradually into higher regions

of the ionosphere. The critical frequency W is that at

which the dielectric penetrability for the ionization density

N, , corresponding to the level of the sharp ionization gradient becomes zero. The effective height of the ionosphere

increases sharply in the transition through WQ and the extinction of waves increases at the same time, since the intensity of the incoming signal is slight. The curves of the

establishment of signals reflected from the E and F regions

with distribution of ionization correspond to the most recent

experimental data. (Met. Abst. 11E-172. )-I.L.D.

D-921 Zhelezniakov, V.V., Radioizluchenie Iupitera. (Radio

emission from Jupiter. ) Priroda, Moscow, 45(3):78-80,

March 1956. 2 figs. , 3 refs. DLC--On the basis of nonRussian papers dealing with radio emission from Jupiter,

the author discusses the discovery of the radio emissions,

the characteristics of the emission curve which resembles

those obtained from thunderstorm electricity discharges at

the earth's surface and suggests that thunderstorm and lightning may occur in the hydrogen atmosphere of Jupiter. (Met.

Abst. 9A-143.)--I.L.D.

334
D-922 Ziegler, H. K. (Signal Corps Eng. Labs. , Ft. Monmouth,

N. J. ), Components for instrumentation of satellites.

(In: Van Allen, James A. (ed. ), Scientific uses of earth

satellites. Ann Arbor, Univ. of Michigan Press, 1956.

p. 55-67. 3 figs. , 6 tables. ) DWB, DLC- -The environmental conditions of satellite instrumentations are re- viewed. Present and predictable availability of suitable

chemical batteries, solar batteries, electron tubes, transistors, and frequency control devices is discussed.

Special attention is given to the comparison of power

sources. (Met. Abst. 9. 4-46. )--Author's abstract.

335
ANONYMOUS

D-923 Akademiebericht uber die Erdsatelliten. (Academy report

on the artificial satellites. ) Osteuropa-Naturwissenschaft,

Stuttgart, 1(2): 155-156, May 1958. DWB--A statement

made by A. W.TOPCHEV at the annual meeting of the Academy of Sciences of the USSR on March 26, 1958, is quoted

from the newspaper Pravda of the same date. The statement refers to preliminary results of atmospheric density,

ionospheric electron density, radio propagation, cosmic

radiation and biological observations made by means of

the first two Soviet Satellites. (Met. Abst. 11J-125.)--

G.T.

D-924 Aktivitat und Kurzwellenstrahlunq der Sonne. (Activity

and short wave radiation of the sun. ) Die Umschau, 53(4):

103, Feb. 15, 1953. 2 figs. DWB--Summary of report of

Radio-astronomy Observatory of Cornell Univ. and McMath

Hulbert Observatory of Univ. of Michigan on correlation

between solar activity and 1. 5 m radiation from flares.

(Met. Abst. 9A-22.)--C.E.P.B.

D-925 Beam of light may carry conversations . C. & P. Call

(Chesapeake and Potomac Telephone Co. ), 32(8):2, Aug.

1961. fig. --By means of the "Optical Maser, " developed

at Bell Telephone Laboratories, the human voice was transmitted for the very first time on a beam of coherent infrared

light. This new mode of communication opens possibilities hitherto not feasible. Space communication may be

one of the multiple applications of the future. --W. N.

D-926 'Bubble' on the Sun. Science and Culture, Calcutta,

21(ll):664-665, May 1956. DLC--Motion picture photographs of the huge solar flare of Feb. 10, 1956 (equal to

100 million H bombs) were shown at Columbus, Ohio, to

American Astronomical Society by scientists from Sacramento Peak Observatory, N. Mexico. The 20, 000 mi

bubble shot out 200, 000 mi at 700 miles/sec, setting a record for solar flares. Most of the gas was hydrogen.

Ultraviolet light from flare affected the ionosphere and

radio transmission. (Met. Abst. 9. 11-164. )--M. R.

336
D-927 Per erste Erdsatellit. (The first earth satellite. ) Naturwissenschaftliche Rundschau, 10(11) :424.42s, Nov. 1957.

2 figs. DWB--Account of satellite launched on Oct. 4,

1957, tracks and structure of radio signals. There is a

brief reference to second satellite which will record ultraviolet solar spectrum, cosmic rays, measurements of

earth's surface and sun's magnetic field. (Met. Abst.

9.2-100.)--C.E.P.B.

D-928 Fourth artificial earth satellite (1958/ff ). Nature, London,

181(4612) :810, March 22, 1958. DWB--On March 17, 1958

the U. S. Navy launched another artificial earth satellite at

Cape Canaveral, Fla. , by means of a "Vanguard" rocket.

The satellite, 1958^ , consisted of an aluminum sphere

6.4 in. in diameter; mass, 3.25 lbs. ; eccentric orbital

revolution, 400 and 2, 500 mi above the earth's surface;

time, 135 min. The satellite is equipped with two radio

transmitters, one powered by chemical batteries, broadcasting on a frequency of 108. 00 Mc/s, the other, powered by

solar batteries, operating on 108. 30 Mc/s. (Met. Abst.

11M12.)-N.N.

D-929 Ionospheric studies using earth satellites. American Geophysical Union, Transactions, 39(1): 169- 174, Feb. 1958.

fig. , table. DWB, DLC-At the USNC-IGY meeting held on

Nov. 5, 1957 at the Central Radio Propagation Laboratory

(CRPL) of the Nat'l. Bur. of Standards, Boulder, Colo. , it was decided that a refinement of experimental techniques

be undertaken. Representatives from 24 laboratories and

organizations were present to give account of their observations of the Russian satellites. Ionospheric turbulence

studied and the fluctuations and fading rates of ionospheric

characteristics were collectively discussed. Recommendations adopted are contained in this report. (Met. Abst.

11E-68. )-N. N.

D-930 International Scientific Radio Union. Nature, London,

178(4532): 528, Sept. 8, 1956. footnote refs. DWB-Review of Proceedings of the 11th General Assembly, the

Hague, Aug. 23-Sept. 3, 1954 (vol. 10 in 5 parts). Pt. 3

deals with Ionosphere radio and Pt. 5 with Radio-astronomy. (Met. Abst. 9A-115. )--C.E. P.B.

D-931 Jupiter emits static (and) Short waves from stars. Science

News Letter, Wash., D.C., 67(16):243, April 16, 1955.

DLC -BURKE and FRANKLIN detected radio noise from

Jupiter that sounded like "thunderstorm interference on a broadcast receiver/' The sferics are heard at 22 Mc

337
about one day out of three during the 6 min when the planet

crosses the narrow path of their radio telescope in Seneca,

Maryland. (Met. Abst. 7. 5-255. )--W. N.

D-932 Long range radio communication by satellite microwave

dipoles. Nature, London, 191(4795): 1237-1238, Sept. 23,

1961. DLC--The West Ford Project, as proposed by the

Lincoln Laboratory, Massachusetts Institute of Technology,

autumn 1959, is an experiment to launch an 8 km wide, and

40 km thick belt consisting of a density of 21 dipoles per

km^, which will reflect radio waves at about 8, 000 Mc/s.

Investigations made by the several committees and the re- sponse from interested scientific groups are reported on,

and the conclusions of the Space Science Board are given

point by point. (Met. Abst. unpub. )--W. N.

D-933 Lunik II — the Russian moon rocket. Current Science,

Bangalore, 28(9) :359, Sept. 1959. DWB, DLC--A short

note on the successful Russian launching of the Moon

rocket Lunik II, which landed on the Moon almost to the

minute according to schedule. The rocket was launched

on the afternoon of Saturday, Sept. 12, 1959. The final

stage of the rocket hit the Moon at 00 hrs, 2 min, 24 sec

(Moscow time) on Monday morning, Sept. 14, 1959.

Launching details and the rocket radio signalings are re- ported. The rocket impact on the Moon as observed from

different observatories is described. (Met. Abst. 11. 12-

182.)-I.S.

D-934 Lunik HI: the Russian third moon rocket. Current Science,

Bangalore, 28(10):393, Oct. 1959. DWB, DLC--A brief

note on the third Russian cosmic rocket launched on Oct. 4,

1959. The multi-stage rocket put into orbit an "automatic

interplanetary station" which, after circling the moon, re- turned toward the earth and is now orbiting the earth. The

significance of this feat for interplanetary exploration is

emphasized and its launching and operation details are given. (Met. Abst. 11. 12-530. )--I. S.

D-935 N. B. S. Research in radio propagation. U. S. National Bureau of Standards, Technical News Bulletin, 38(4):49-59,

April 1954. photos. DLC--A brief review of the work of

the Central Radio Propagation Laboratory, which has four

main divisions: (a) the Ionosphere Research Laboratory,

whose investigations include solar rf radiation, upper atmospheric winds, etc. ; (b) the Systems Research Laboratory, which is concerned with tropospheric propagation

and with research on the best use of the frequency spectrum;

338
(c) the Measurements Standards Laboratory, which is re- sponsible for the standard frequency broadcasts from

WWV and WWVH; (d) the propagation prediction services.

(Met. Abst. 6D-256. )--I. R.E. , Proceedings, No. 3018,

Nov. 1954.

D-936 O zapuske kosmicheskoi rakety v storonu Luny (iz soobshchenii Tass). (Launching of a cosmic rocket toward the

Moon (from TASS announcements). ) Priroda, Moscow, No.

1:I-IV, Jan. 1959. DLC--On Jan. 2, 1959, the USSR launched a multistage rocket toward the Moon. The final stage of

the rocket, which weighed 1, 472 kg without fuel, was provided with a special container which contained instrumentation for the following investigations, viz. : determination

of the Moon's magnetic field, radiation intensity and variation of intensity of cosmic rays, determination of lunar ra- dio activity, etc. For observations on the flight of the final

rocket stage it contained a radio transmitter, broadcasting

on 19, 997 and 19, 995 mHz telegraphic messages 0. 8 and

1. 6 seconds long, a radio transmitter on a frequency of

19, 993 mHz broadcasting scientific data, a transmitter with

a frequency of 183. 6 mHz used for measuring parameters of

motion and broadcasting scientific data, and special apparatus for making a Na cloud. The course of the rocket and the

nature of the signals transmitted for approximately 3 hr intervals from 0300 h (Moscow time) Jan. 3 to 10:00 h Jan. 5,

1959, is described. The cosmic rocket went into the periodic orbit of an artificial satellite on Jan. 7-8, 1959. (Met.

Abst. 11. 12-181. )--I.L.D.

D-937 Planets emit radio waves. Science News Letter, 69(24):

374, June 16, 1956. DWB, DGL--Two types of radio frequency radiation are emitted from planets (Venus and Jupiter). They are caused by 1) heat absorbed from sun's rays

and re-radiated and 2) electrical storms similar to thunderstorms. The temperature of Venus was found to be > 212

although from optical methods a temperature only half that

high was deduced. The latter applies only to the top of

the Venus cloud layer, whereas the radio frequency waves

indicate temperatures deep down in the cloud layer or perhaps at the surface of the planet. (Met. Abst. 9A-128.

)

--M.R.

D-938 Progress Chekhoslovatskoi astronomii v 1945-1955 q. q.

(Progress of Czechoslovak astronomy from 1945-1955.)

Bulletin of the Astronomical Institutes of Czechoslovakia,

Prague, 6(3, 4):41-64, 65-96, 1955. bibliog. at end of

each section. In Russian and English. DLC--

339
Literature published in Czechoslovakia in the field of

astronomy during the period 1945-1955 is reviewed in 8 sections (each written by different authors) with references

(amounting to a total of some 300) at the end of each section. Information of meteorological interest is contained

in the following sections (papers in Russian and English):

Bumba, V. , Fizika solntsa. (Solar physics), p. 41-52 (106

refs. ). Includes chapter on solar effects on the general

circulation of the atmosphere and on the state of the upper

atmosphere, with some 30 refs. Guth, V. , Meteornaia

astronomiia, (Meteoric astronomy), p. 65-76 ("78 refs.

)

with chapters dealing with upper air density determination

by means of meteors; meteoric ionization and meteoric

dust in the atmosphere (23 pertinent refs.). Ceskoslovenska Akademie Ved. Astronomicky Ustav, Vysokie sloi atmosfery. (The upper atmosphere), p. 76-82 (42 refs.). In

this paper various astronomical techniques (used in

Czechoslovakia) for research on the upper atmosphere are reviewed: namely observation of the earth's shadow during lunar eclipses (ozone, meteoric dust); measurement of

twilight spectra, and ionospheric soundings. Other sections are on: Celestial mechanics; Comets (with reference to LINK's paper on correlation between discovery of

comets in historic times and climatic changes); Astrometry;

Stellar astronomy and Radio astronomy. (Met. Abst. 7. 10-

38.)-G.T.

D-939 Put' v kosmos: materialy gazety "Pravda" o trekh sovetskikh iskusstvennykh sputnikakh Zemli . (Journey into space:

material from "Pravda" on the three Soviet artificial earth

satellites.) Moscow, Izdat. "Pravda," 1958. 319 p. figs.,

photos. DWB--A popular book (50, 000 copies) consisting

of about 70 articles, many by top scientists or academicians, on the 3 Soviet sputniks and their scientific results

to date. The articles are grouped into 6 chapters: (1) the

first Soviet artificial satellite, (2) comments by scientists

in the U. S. S. R. , (3) comments from foreign scientists,

(4) the second artificial satellite, (5) some notes on the

scientific results of the first sputniks, (6) the third Soviet

satellite. (Met. Abst. 10. 4-77. )--M. R.

D-940 Radioastronomicheskie izmereniia napravleniia i skorosti

vetrov v vysokikh sloiakh atmosfery. (Radio-astronomic

measurements of direction and velocity of winds in upper

atmospheric layers. ) Uspekhi Fizicheskikh Nauk, Moscow,

48(1): 138-143, Sept. 1952. 2 figs. , 9 refs. DLC--Review

based mostly on foreign papers, emphasizing the use of

"radio stars " in measuring fluctuations due to ionospheric

340
disturbances. Tentative data for dimensions of disturbances, drift direction and speed and vertical velocity

given. Wind roses and histograms for wind frequencies

in F2 layer are presented for: a) May-June 1951 at 60 N

and b) Sept. -Oct. 1951 at 53°N. Data compiled for var- ious levels 80-250 km for U. S. A. , England, Germany and

Australia. (Met. Abst. 4F-115. )--A. A. , M. R.

D-941 Radio signals from Mars. Science, Wash., D. C.

124(3223) :620, Oct. 5, 1956. DLC--U. S. Navy announced

detection of first radio waves from Mars, picked up with

a 600 in. radio telescope at National Research Lab. in

Washington, D. C. (where first radio signals from Venus

were detected earlier in 1956). Emissions indicate an

average temperature of Mars of slightly below 32^F. The

3 cm signals were picked up on 2 nights in early Sept.

1956. (Met. Abst. 9A-130. )-M. R.

D-942 Relations between the sun and the ionosphere . Nature,

London, 179(4564) :804-806, April 20, 1957. DWB«Account of Geophysical Discussion at R. Astron. Soc. , Feb.

22, 1957. The first part was on "The great solar flare of

Feb. 23, 1956", with increase of cosmic rays, radio

fadeout and other phenomena even on dark side of the

earth, indicating a sudden increase of ionization at 80-

90 km about 0345 UT. The second part dealt with 'The

solar cycle variation of the sun's ionizing radiation."

separating the background from a slowly varying component from local active centers. (Met. Abst. 8.7-318.)--

C.E.P.B.

D-943 Research based on Sputniks I and II reported by Soviets.

Science, Wash., D.C., 127(3311): 1378-1381, June 13,

1958. DLC --Excerpts from the article Soviet artificial

earth satellites which the Soviet Embassy, Wash. , D. C.

released May 19, 1958. The popular article is based on

results as published in Pravda, April 27, 1958. It is

stated that scientific papers are to be published in various journals. The highlights may be summed up as follows: The density of the upper layers of the atmosphere

at 225-228 km appears to be 5 to 10 times greater than

theoretical values before sputniks. Changes of the state

of the atmosphere as dependent on latitude and time of

day are assessable. The temperature at 225 km altitude

was higher than shown by pre-sputnik theories and higher

than solar influence may yield. Determination of electron

densities are predictable from known deflection of the ra- dio beam. Cosmic ray particle number can be determined

341
as dependent on altitude. The increase was about 40%

from 225 km - 700 km altitude. Variation of intensity

which is believed to relate to the interplanetary environment near the earth may be checked by the now possible

cosmic ray "sounding" of the earth's magnetic field at

very great distances from the globe. Electrocardiograms,

obtained from the first dog in space, revealed no morbid

symptoms, the heart beat diminished frequently due to increase of the acceleration. The weightlessness in orbit

was taken quite well, movements were brief and rather

smooth. (Met. Abst. 11J-143. )--W. N. ^

D-944 Rocket flare patrol program. American Geophysical Union,

Transactions, 39(1): 165-167, Feb. 1958. table. DWB, DLC

--Summary of the scientific results of the rocket flare patrol

program, giving the dates, altitude in feet, physical appearance of the sun, data obtained and comments on particular

observations. Advances in rocket launching have now led

to a perfect telemetering performance on all flights because

of the use of the new type of aerodynamic telemetering an- tenna, with uniform radiation pattern. Several scientific

rocket results correlated with direct solar observations have

proved real and practicable. (Met. Abst. 11. 4-149. )--N. N.

D-945 Satellite communication. Institution of Electrical Engineers,

Journal, 7(80) :487-488, Aug. 1961. DLC-The USA satellite

Echo I communication experiments in 1960 improved and ex- panded the busy and often disturbed frequency bands <30

Mc heretofore used, by establishing non-interference transcontinental and transoceanic radio communication between

1000 and 10, 000 Mc. Some of the several technical, operational and international problems thus arisen, along with

further satellite communication tests planned in 1962 on an

international basis, are outlined briefly. The problems are now being examined by Study Group IV of the International

Radio Consultative Committee of the International Telecommunication Union pending an interim meeting early 1962 in

U. S. A. and the 10th Plenary Assembly of C. C. I. R. in 1963.

-W. N.

D-946 Solar eclipses and the ionosphere: a symposium held under

the auspices of the International Council of Scientific Unions

Mixed Commission on the Ionosphere, in London, Aug. 1955. Editors, W. J. G. Beynon and G. M. Brown. London, Pergamon,

1956. 330 p. figs. , tables, eqs. , refs. at end of each ch.

Literature on solar eclipses and the ionosphere (including)

chronological catalogue of eclipses, p. 308-320 (225 refs.).

Issued as Vol. 6 of the Special Supplements to the Journal of

342
Atmospheric and Terrestrial Physics. Articles abstracted

separately. DWB. Review by R. M. Goody in Weather,

12(6):198, June 1957. Review by R.L. Smith-Rose in Nature,

London, 179(4562): 711, April 6, 1957. Also: Beynon, W.

J. G. , Solar eclipses and the ionosphere.

D-947 The space encyclopedia: a guide to astronomy and space

research. N. Y. , E. P. Dutton, 1957. 287 p. numerous figs.,

photos, tables. Appended: Nov. 1957 Supplement. 5 p.

DWB (629. 1388 S732)--A glossary of terms used in all fields

of astronautics, space medicine, and associated astrophysical, geophysical and meteorological phenomena, arranged

alphabetically, with many fine illustrations of equipment and

results and observations. Such unrelated terms as zodiacal

light, radar, solar prominences, falling sphere, galaxies,

atmosphere, origin of earth, earth as seen from space, artificial earth satellite, etc. , are described and illustrated.

An appendix of 5 pages includes a description and illustration of the first Soviet Sputnik (Oct. 4, 1957), and the U. S-. "Farside " Rocket which was shot on Oct. 21, 1957, reaching

4000 mi. (Met. Abst. 10. 4-73. )--M. R.

D-948 Scientists upset theories about particles in space. The

Evening Star, Wash. , D. C. , A-ll, June 11, 1957. -Radio

propagation experiments indicate that the "ghost signals " arriving about 3/4 sec later, come from space up to 6000

mi. The findings of ROBERT A. HELIWELL and his associate ERNST GEHRELS (both of Stanford Univ. ) contradict

current theories on magnetic storms, aurora borealis, and

deepen the problems of solar activity as influencing weather.

Outer space may be utilized for radio communication. (Met.

Abst. 12B-150.)--W. N.

D-949 The second U. K. Scout satellite. Nature, London, 190

(4777):681, May 20, 1961. DWB-The payload for the second

U. K. Scout satellite has now been agreed. A project to measure the galactic noise in the frequency range 0. 75-3 Mc/s

and the exploration of the upper ionosphere will be carried

out by Dr. F. Graham Smith, Mullard Radio Astronomy Observatory, Cavendish Laboratory, Cambridge. Two methods

of measuring atmospheric ozone will be directed by Dr. R.

Frith and Dr. K. H. Stewart of the Meteorological Office,

Great Britain. The measurement of micrometeorite flux will

be organized by Dr. R. C. Jennison of Jodrell Bank. --R. B.

343
D-950 Solar flare of May 20. 1959. Sky and Telescope, N. Y. , 18(10): 544-545, Aug. 1959. photos. DWB# DLC--An illustrated discussion of the solar flare of importance 3 which

occurred on May 10, 1959. This flare ranks as one of the

largest and brightest yet observed. It occurred in the vicinity of a spot group on the northeast quadrant on the sun, fairly

near the limb. Simultaneously with the appearance of the

flare, there also began a sudden enhancement of atmospherics.

Two photographs, one photographed in red light of hydrogen

and the other a monochromatic picture illustrate the description. The record of radio bursts obtained on May 10th at the

Harvard Radio Astronomy Station in Texas is also photographically shown. Other phenomena probably induced by this gigantic flare are described. (Met. Abst. 11L-270. )--I. S.

D-951 The solar flare of Feb. 23. 1956. Discovery, 17(5): 177-179,

May 1956. 4 figs. DLC- -Increasing area of sunspots occur- red in Feb. 1955 and a large flare on Feb. 23, 0330-0510 UT

at Kodaikanal. An increase of about Q% in cosmic radiation

was reported. There was a complete fadeout of short wave

radio. (Met. Abst. 11E-154. )--C. E.P.B.

D-952 Soviet writings on earth satellites and space travel. N. Y.

,

Citadel Press, 1958. 253 p. 41 figs. , tables. DWB, DLC--

The history of Russian development of astronautics and rocketry (since 1924) leading up to the successful launching of

the first Sputnik on Oct. 4, 1957, is recounted, followed by

general aspects of rockets, satellites and space travel and

uses thereof. A Joint Committee on Space Travel was organized in the Astronomical Council of the Akademiia Nauk in

1954 and an Astronautical Society at the Central Air Club in

Moscow (also 1954). The International Astronautical Federation coordinates societies of > 20 countries. Pt. II includes a number of articles or interviews with Soviet scientists after Sputniks I, II or III were launched, and covers

many aspects of satellite observations and applications

(military# communications, optical, weather (OBUKHOV),

astronomical, solar, travel to moon or planets, biological

problems, navigation, power, etc.). (Met. Abst. 11.1-110.)

--M.R.

D-953 Space Science Board (of National Academy of Sciences - National Research Council). Science, Wash. , D. C.

,

128(3320) :350-351, Aug. 15, 1958. DLC-The 16 man Space

Science Board as established by the National Academy of

Sciences, National Research Council, has assumed the task

"to survey in concert the scientific problems, opportunities

and implications of man's advance into space" under the

344
chairmanship of LLOYD V.BERKNER. Activities and functions of the Space Science Board will be subject for coor- dinations and cooperation with similar domestic and foreign

civil and government bodies. The 11 Ad Hoc committees or- ganized are: 1) Geochemistry of space and exploration of

moon and planets. 2) Astronomy and radio astronomy. 3)

Future vehicular development. 4) International relations

field. 5) Immediate problems. 6) Space projects. 7) Ionosphere. 8) Physics of fields and particles in space. 9)

Future engineering development beyond available facilities.

10) Meteorological aspects of satellite and space research.

11) Psychological and biological research. The names of

the chairmen of the different committees are listed. (Met.

Abst. 11M45.)-W.N.

D-954 To study whistlers. Science News Letter, Wash. , D. C.

,

67(l):3f Jan. 7, 1956. DWB, DLC-Whistlers, which are radio waves of audiofrequency that are bom of individual

lightning impulses, will receive special attention during

the International Geophysical Year, 1957-1958. Whistlers

are not the same as cosmic noise due to radio waves from

outer space. The so-called "dawn chorus," a radio effect

connected with the aurora and magnetic disturbances and

caused by the bombardment of the earth by material shot

from the sun, will be also listened to. It is hoped that this

will settle what comes from the sun to disturb radio, TV and

wire communications on the earth, particularly at the time of

the greatest prevalence of sunspots. (Met. Abst. 8. 3-348. ) -A.M. P.

D-955 Twinkling of stellar radio waves studied. Science News

Letter, 68(1): 3, July 2, 1955. DLC-Preliminary studies by

C.GORDON LITTLE show a marked difference between the

way radio stars twinkle in England and in Alaska. Size,

shape and movement of the dense regions in the ionosphere

are indicated by the twinkling. (Met. Abst. 7.4-285.) — W.N.

D-956 Two major observatories join in solar studies. Science News

Letter, Wash. , D.C., 27(21):327, May 21, 1955. DLC--

The explosive energy of the sun and its impact on all atmospheric layers will be jointly studied by the Smithsonian Institution and Harvard University. The subject has great

theoretical interest for astronomers and geophysicists and

is of practical value in radio communication, weather forecasting and rocket flights. Headquarters of the Astrophysical Observatory is being moved from Washington, D. C. to

Cambridge, Mass. , as of July 1, 1955. (Met. Abst. 7. 5-21. ) -W. N.

345
D-957 Union Radio Scientifiaue Internationale (U. R. S. I. ). (International Scientific Radio Union. ) International Union of

Geodesy and Geophysics, Bulletin d'Information, 2(2): 362-

370, April 1953. DWB-First assembly in Sydney, Australia

under Presidency of Sir EDWARD APPLETON, Aug. 11-21,

1952, attended by 300 delegates, 50 from overseas. Commissions dealing with measurements, tropospheric waves,

ionospheric waves, sferics, radio astronomy, etc. , met

during the session. It was decided not to publish the documents presented at the meeting but to publish Special Reports of the U. R. S. I. from time to time on such subjects

as ionospheric storms, meteors, wave interaction, etc.

(Met. Abst. 6D-217,)--A.A.

D-958 U. S. Moon Rocket Pioneer IV. Current Science, Bangalore,

28(3): 100, March 1959. DWB, DLC-The U.S. four-stage

Juno II rocket was launched on March 3, 1959 from the Cape

Canaveral missile test center (Florida). It carried a 13.4

lb gold plated space probe, Pioneer IV. At 22. 24 hrs GMT

on March 4, the space probe by-passed the moon at a distance of 37, 771 miles from it. This is more than 17, 000

miles further away than was planned. Data were received

on the telemeter by Jodrell Bank and the Goldstone tracking

stations until March 6. By then it had gone 406, 020 miles

from the earth and was travelling at 3899 mph. (Met. Abst.

11. 12-524. )-N.N.

346
SUPPLEMENTARY MATERIAL

D-959 Allcock, G. McK. and Rodgers, M. F. (both. Dominion

Physical Lab. , Lower Hutt, New Zealand), Geomagnetic

activity and the reception of whistlers in polar regions.

Journal of Geophysical Research, Wash. r D. C. , 66(11):

3953-3955, Nov. 1961. fig., table, 5 refs. DWB, DLC--

The negative correlation between whistler reception and

geomagnetic activity at geomagnetic latitudes of 5G and

66 (Barrington, 1960) was found stronger as the auroral

zone was approached and even more pronounced at the

Scott Base (79 S) Antarctica. A strong diurnal variation

in whistler reception was found but not significant seasonal variation in the shape of diurnal curves. --S. N.

D-960 Australia. Commonwealth Scientific and Industrial Research Organization. Div. of Radiophysics, Radio

astronomy bibliography, 1954-1956. Sydney, Aug. 1957.

292 p. 1016 titles with brief summaries, arranged by

subject. List of journals (with abbreviated titles) re- ferred to, p. xiii-xxv. Author index p. 279-292. 'Transcript of accumulated card entries from the CSIRO Radio

physics Abstracts, for 1954-1956. Similar publication

covering 1952-1954 issued in 1954 with limited circulation. These two issues constitute a tentative bridging

of the gap between existing and projected publications

of Cornell Univ. Bibliography of extraterrestrial radio

noise. " (See ref. D- 107, 108. ) (Met. Abst. unpub.

)

D-961 Bain, W.C. (Radio Res. Station (DSIR ), Slough), What

space research is revealing about the ionosphere. New

Scientist, London, 12(262):493-495, Nov. 23, 1961. 6

figs. DWB--The different techniques used for measuring

ionospheric characteristics by means of artificial satellites are reviewed, namely those based on 1) the Faraday effect;

2) the Doppler effect; 3) scintillation of radio signals and

4) direct measurement with various probes. Important re- sults already achieved with these techniques include confirmation of the discovery (originally made by Moon radar)

that the number of electrons above the F region is about 3

times the number below, and the discovery (as a result of

Canadian rocket measurements) that electron collisional

347
frequencies in the D and E regions are several times smaller

than believed previously. Plans for "topside sounder" satellites are mentioned which are hoped to provide much more

information about the ionosphere than the satellite measurements made heretofore. --G.T.

D-962 Bauer, Siegfried J. and Daniels, Fred B. , Ionospheric

parameters deduced from Faraday rotation of lunar radio re- flections. Journal of Geophysics, Wash. , D. C. , 63(2):

439-442, June 1958. fig. , 7 refs. , eqs. DWB--Faraday

rotation at 151. 11 Mc/s was measured in 30 steps Jan. 8-9,

1958 from 23. 30 to 05. 30 CST. The lunar reflected transmissions from Belmar, N. J. , were received at Urbana, 111.

The observed results: 7. 7 x 10^2 electrons cm"2 are compared with the computed results: 3. 5 x 10^2 electrons cm"2

of a parabolic layer model, using Fort Monmouth, N. J. data.

There are on the average, during night, 3. 4 times as many

electrons above as below maximum. (Met. Abst. unpub. ) --W. N.

D-963 Becker, W. (Inst, fur Ionospharen-Physik, Germany), The

varying electron density profile of the F region during magnetically quiet nights. Journal of Atmospheric and Terrestrial Physics, London, 22(4):275-289, Dec. 1961. 12 figs.,

8 refs. DLC--Ionograms taken at Lindau and at two field

stations (average distance from Lindau 125 km) on magnetically quiet nights were reduced to N(h) profiles of the Flayer. The normalized profiles showed maximum height

changes of about 60 km lasting for about 2 hrs; they also

showed layer height differences on comparable nights of

more than 100 km . No seasonal influence on the rise and

descent of these profiles in the late evening and early morning hours, respectively, could be found. The ionograms of

the field station showed no local difference or temporal displacement. Generally, the electron loss rate at the F layer

peak is closely related with the height of the peak and,

therefore, dependent on season. Spread F echoes of high

intensity are occasionally observed at Lindau even on magnetically quiet nights; they are not necessarily associated

with vertical movements of the F layer. No spread F echoes

were observed during vertical movements of the F layer induced by positive magnetic bay disturbances. It is not possible to determine from either observation whether vertical

movements cause unstable conditions within the F layer.

--Author's abstract.

D-964 Benson, Robert F. (Univ. Alaska), Effect of line of sight aurora on radio star scintillations . Journal of Geophysical

Research, Wash., D. C. , 65(7): 1981 -1985, July 1960.

4 figs., 5 refs. DLC--

348
Evidence is presented to show that active auroral forms that

pass across the line of sight to a radio star can have a direct effect on the scintillations of the signal received on a frequency of 223 Mc. This effect is most pronounced if the

level of scintillation activity is relatively low before the aurora crosses the star position. Two examples are presented: in the first, an intense auroral band between the radio

source in Cassiopeia (angular diameter, 4* ) and the receiver

disrupts the characteristic sinusoidal trace produced by the

radio star signal in the output of the phase switch interferometer. This long duration fade lasted for a period of about

8 min. In the second example, the aurora is accompanied

by strong angular scintillation coincident with strong absorption of 27.6 Mc galactic radio waves. In both examples

the radio star was within 10 of the geomagnetic zenith.

(Met. Abst. 12A-27.) -Author's abstract.

D-965 Bhargava, B.N. (Kodaikanal Obs. , Kodaikanal), Observations of spread echoes from the F layer over Kodaikanal: a preliminary study. Indian Journal of Meteorology and Geophysics, New Delhi, 9(1): 35-40, Jan. 1958. 5 figs. , 10

refs. DWB, DLC- Occurrence of spread F echoes at Kodaikanal for a period of about one year has been analyzed and

diurnal and seasonal characteristics have been found to exist in the frequency of occurrence of these echoes. It has

been found that the phenomenon occurs only during nighttime,

with largest frequency between 1900 and 0400 hrs local time.

While the seasonal variation is characterized by equinoctial

maxima as in the case of geomagnetic activity, the day-today variations in scattering indicate a negative correlation

with the degree of magnetic activity. Thus, scattering persists for largest percentage of time during comparatively

quiet periods and is often altogether absent on magnetically

stormy nights. The phenomenon is discussed in relation to

ionospheric irregularities and radio star scintillation. (Met.

Abst. 9. 10-165. ) -Author's abstract.

D-966 Bolton, J. G. ; Slee, O.B. and Stanley, G. J. , Galactic

radiation at radio frequencies, Pt. 3. The sea interferometer.

Pt. 6, Low altitude scintillations of the discrete sources.

Australian Journal of Physics, Melbourne, 6(4):420-451,

Dec. 1953. figs. , tables, refs. DLC--In Pt. 5, the factors

involved in the study of discrete sources of galactic noise

by the sea interferometer are discussed. Three new forms of

sea interferometer which increase the effectiveness of this

technique are described. Pt. 6 represents a study that has

been made of the scintillations of four discrete sources at

altitudes of from to 10 . The observations cover the years

1947-1951 and were made at various frequencies in the range

349
40-300 Mc/s. It was found that the scintillation index, a measure of the amplitude of the scintillations, (1) increases

with increasing wavelength, (2) decreases rapidly with increasing altitude, (3) shows seasonal and diurnal variations,

the seasonal component having minima near the equinoxes

and the diurnal component having minima near the equinoxes

and the diurnal component near dawn and sunset. The scintillation rate, or the number of scintillations per minute (1)

is different for sources of different declination, (2) is independent of wavelength. In the case of the Cygnus source,

the data for which are the most extensive, the rate increases

and the decline in the scintillation index with altitude is

less rapid during the winter months. A strong correlation

is established between the occurrence of the scintillations

and sporadic E. The difference in the scintillation rates for

different rates for different sources can be explained in

terms of variations in the size of irregularities and the effects of the winds in the Es layer. (Met. Abst. 9A-25.

)

--Authors' abstract.

D-S67 Braude, S. la. , K voprosu o vybore etalonnogo diskretnoqo

istochnika kosmicheskoqo radioizlucheniia. (On the selection of a standard discrete source of cosmic radio emission.

)

Astronomicheskii Zhurnal, Moscow, 38(5):898-904, Sept./

Oct, 1961. 4 figs. , 2 tables, 20 refs. , 6 eqs. Russian and

English summaries p. 898. Transl. into English in Soviet

Astronomy AJ, New York, 5(5):687-691, March/April 1962.

DLC--The possibility of using the discrete radio source Cygnus A as a standard is considered. The procedure and cor- rections, due to the proximity of the extended source Cygnus

X, are given. The flux density of radio emission for the

standard source in Cygnus A in the frequency range 12. 5 - 10, 000 Mc/s is determined. The discordancies of the data,

found by different authors, for the flux density of radio emission on frequencies lower than 30 Mc/s are noted. --Author's

abstract.

D-968 Briggs, B. H. (Cavendish Lab. , Cambridge), Correlation of

radio star scintillations with geomagnetic disturbances . Geophysical Journal, London, 5(4):306-317, Oct. 1961. 5

figs. , 21 refs. , 3 eqs. DWB, DLC--The correlation between

the degree of scintillation of the radio source Cassiopeia A

and the local magnetic K index is studied. It is shown that

the correlation coefficient between these quantities depends

upon the epoch of the solar cycle at which the observations

are made, on the position of the source in the sky, and on

the radio frequency used. For observations on 38 Mc/s

made at sunspot minimum, the correlation coefficient is

small but positive for all positions of the source. At

350
sunspot maximum, the correlation coefficient is positive

when the source is near upper transit and negative when

it is near lower transit; the average value of the correlation

coefficient for all positions of the source is approximately

zero. It is shown that these results can be explained when

the finite angular diameter of the radio source is taken into

account. For some conditions an increase in the degree of

irregularity of the ionosphere can result in a decrease in the

degree of scintillation which is observed. It is suggested,

therefore, that the degree of irregularity of the ionosphere

always increases during magnetic disturbances in medium

latitudes, and that the negative values of the correlation

coefficient between scintillation index and magnetic K index

which are sometimes obtained are due to a secondary effect

related to the finite size of the source. The results of the

present paper explain the inconclusive and conflicting re- sults of earlier workers. --Author's abstract.

D-969 Buck, Richard F. , Provide services toward instrumenting

Aerobee rockets . Oklahoma. State Univ. Research Foundation, Contract AF 19(604)-2029, Final Report, July 31, 1980.

40 p. 13 figs. DWB--Contract AF 19(604)-2029 has represented a continuation of a series of support contracts between the Research Foundation Electronics Laboratory of

Oklahoma State University and the Air Force Cambridge Research Center. A wide variety of support activities have

been conducted throughout the period of this contract. The

logical breakdown of these activities separates them into

two broad classes: (1) direct support in the form of manpower and equipment for bunch missions at the firing sites,

where upper air research experimentation has been conducted

through the use of rocket sounding vehicles, and (2) indirect

support activities, which have been concerned with activities

in the Stillwater laboratory. These have provided the necessary equipment and facilities for these research instrumentation vehicles. Direct support activities for rocket borne

equipment have been concerned with L band beacons, FM/FM

telemetry systems, Range Safety equipment for tracking and

flight termination, preparation of actual payload structures,

and other miscellaneous activities related to the installation,

check-out and operation of all of these forms of equipment.

Further direct support activities have been concerned with

the construction and operation of necessary ground receiving

equipment for L band transponder beacons, SMT telemetry

systems, special telemetry systems utilizing special pulsetime modulation of telemetry pulses following a normal S - band tracking beacon, FM/FM recording equipment, and

blockhouse activities associated with the launch and prelaunch periods for all of the above types of equipment.

351
Indirect support activities have been considerably more

varied in nature. In many cases investigations and circuit

development programs have led to improvements of existing

equipment, or construction of more modern replacement

equipment, in order to provide the necessary ground installations required for support and to improve performance of the

air borne components in use. Some of the equipment involved has been designed completely and constructed by

this organization; in other instances commercially available equipment has been purchased and integrated into systems compatible with the rocket experimentation program.

In addition to the equipment provided for continued field

operation and support activity, a separate program in the

Stillwater laboratory has resulted in the design and construction of a single prototype transistorized pulse-time to

DC -data converter unit which is capable of transforming re- ceived pulse-time telemetry signals into suitable form for

strip chart recording. The final circuit of this prototype

data converter is discussed in some detail and an estimate

presented of the greater improvements possible within the

present state of the art, if this investigation should be continued. --Author's abstract.

D-970 Castelli, John P. ; Aarons, Jules; Ferioli, Carl and Casey,

Joseph (all, U. S. Air Force, Hanscom Field, Bedford, Mass.),

Absorption, refraction, and scintillation measurements at

4700 Mc/s with a traveling wave tube radiometer. Planetary and Space Science, N. Y. , London, l(l):50-56, Jan. 1959.

7 figs. , 2 refs. DLC--By means of radio astronomy techniques, measurements of atmospheric absorption were made at

C band (4700 Mc/s), with the sun as a source of radio frequency energy. The equipment, a comparison type radiometer, used travelling wave tubes, a tuned radio frequency

receiver, and an altazimuth antenna mount. The average

solar temperatures recorded for the period varied from

22, 000°K at zero elevation to 26, 000°K at 60° of elevation.

Individual readings ranged between 18, 000 K and 30, 000 K.

The mean absorption, based on average solar temperatures

at the various elevations for the period, was 0. 00348 dB/km.

Refractive errors were approximately the same as optical although deviations from the mean during any day were large.

Atmospheric scintillation for periods ranging from 0. 5 sec

to 90 sec were recorded. Scintillation amplitudes ranged

from 2% to 20% of antenna signal temperature at low angles.

At high elevation angles, scintillations rarely reached 10%

and were generally less than 1%. (Met. Abst. 13.4-387.)

--Authors' abstract.

352
D-971 Chapman, J. H. and Molozzi, A. R. (both, Defence Research Telecommunications Establishment, Ottawa), Interpretation of cosmic noise measurements at 3. 8 Mc/s from

satellite 1960 1 . Nature, London, 191(4787):480, July 29,

1961. 2 refs. DWB, DLC--The results of measurements of

cosmic noise at 3. S Mc/s from the satellite 1960 1 showed

variations in field strength at different locations. These re- sults have now been analyzed, on the assumptions that the

variations in signal strength are due to three causes: (a) the

variation of radiation resistance of the antenna due to the

ionosphere surrounding the satellite; (b) the restriction in

angular aperture of the satellite antenna due to the ionosphere; and (c) the variation of cosmic noise over the sky.

The results indicate that these are the most important factors affecting the cosmic radio noise. --R.B.

D-972 Conway, R.G. ; Shuter, W.L.H. and Wild, P. A. T. (all,

Nuffield Radio Astron. Labs. , Jodrell Bank), An attempt to

observe radio emission from Comet Burnham 1959 k. Observatory, London, 61(922): 106-107, June 1961. 2 tables, 4

refs. , eq. --It seems uncertain whether radio emission by a comet has yet been observed. During the recent close approach of comet Bumham (1959 k) an attempt was made with

the Jodrell Bank radio telescope to reach for radio radiation

but none was observed. A table summarizes the observations. --S. N.

D-973 Dagg, M. , Radio star ridges . Journal of Atmospheric and

Terrestrial Physics, 11(2):118-127, 1957. 4 figs. , 3 tables,

8 refs. DWB--A radio star "ridge" effect has been investigated which is quite different in character from the usual

radio star scintillations. The occurrence of ridges correlates

more closely with ionospheric inhomogeneities in the E re- gion than in the F region. A divergent lens mechanism for

the production of ridges is proposed which gives a qualitative explanation of the main features. (Met. Abst. 9A-146.)

--Author's abstract.

D-974 Douglas, J. N. and Smith, H. J. (both, Yale Observatory,

New Haven, Conn.), Presence and correlation of fine structure in Jovian decametric radiation . Nature, London, 192

(4804):741, Nov. 25, 1961. fig., 11 refs. DWB, DLC--

Four identical crystal controlled total power receivers working at 22, 200 Mc/s with 6 kc/s bandwidth were set up at

Yale University's Bethany Observing Station and three other

stations at distances of 15, 30 and 100 km. from Bethany.

These were used during March to August 1961 to observe

the radio noise storms in the Jovian non-thermal emission.

Correlation between the records at the different stations

353
varied during the period of the observations, but on six

nights the correlation was essentially perfect. It is concluded that the fine structure of these emissions is characteristic either of the source at Jupiter or of the interplanetary medium. This intrinsic structure is often obliterated by

local ionospheric effects. --R. B.

D-975 ElgarpV, 0ystein, High resolution spectrometry of enhanced

solar radio emission. Astrophysics Norvegica, Oslo, 7(5):

123-263, Sept. 1961. 94 figs. , 6 tables, 95 refs. , 19 eqs.

DWB, DLC--A sweep frequency receiver of high resolving

power is described. The sweep is repeated 50 times per sec

in the frequency band from 215 to 190 Mc/s. The instrument

has been used to investigate the fine structure of solar radio

emissions. From a number of observations of bursts of spectral type I it is concluded that the dynamic spectra of this

class of bursts take various forms. For practical reasons a subdivision of the type I class is made for use in the present paper. The frequency of occurrence of bursts in the different sub-classes is determined from some representative

noise-storm records. Lifetime, band width and line profile

of type I bursts are studied. Some observational evidence

of echo effects is presented. Examples are shown of bursts

that are split into two components with a frequency separation of about 8 Mc/s. This is likely to be the same type of

splitting known from bursts of spectral type II (outbursts).

Theories proposed to explain type I storms are reviewed and

compared with observational results. Some interpretations

of the sweep observations are proposed. Arguments are advanced in support of the view that type I bursts are generated by a sporadic emission process with energy output in a narrow frequency band, as opposed to the suggestion that

the bursts are caused by variable transmission or focusing

of radiation from a wide band source. Some examples are shown of solar radio emissions with peculiar structure, and

possible interpretations are discussed. High resolution

spectra of type III bursts recorded at the Oslo Solar Observatory are compared with wide band spectra obtained simultaneously at the Harvard Radio Astronomy Station. The agreement between the records is very good. Evidence is presented of fine structure in type III bursts. It is possible to

account for the details in the type III burst spectra on the

basis of current theory for this class of solar radio events.

--Author's abstract.

3S4
D-976 Eshleman, V. R. ; Gallagher, P. B. and Barthle, R. C. (all,

Radioscience Lab. , Stanford Univ.), Radar methods of

measuring the cislunar electron density. Journal of Geophysical Research, Wash., D.C., 65(10):3079-3086, Oct.

1960. 16 refs. , 10 eqs. DLC--The ionized medium between

the earth and the moon is being studied at Stanford by means

of lunar radar echoes. Of prime interest is the electron density beyond the earth's ionosphere, in regions (at distances

of several to 60 earth radii) where the interplanetary gas

may be dominant. Six related techniques for measuring the

total integrated electron density are discussed. In practice

the ionospheric part could be determined separately and subtracted from the total. These same techniques could be used

to measure by radar the electron density between the earth

and various planets, and to measure by one-way propagation

the integrated electron density between a space probe and

the earth. The moon's radar range exceeds the true range,

especially at low frequencies, because of group retardation,

which is a measure of integrated electron density. Density

measurements based on absolute measures of radar range

would require very high peak power (for pulse ranging) or very high equipment stability (for CW ranging); furthermore,

the true lunar range is not known accurately. In two of the

methods described here, the full average power capability

of the transmitter can be used without need for high stability

or precise knowledge of the lunar range. In effect, a reference is sent with the measuring quantities and only relative

radar range is measured. Doppler frequency shifts and the

earth's magnetic field cause only slight difficulties. However, path splitting, electron "blobs," and lunar surface

irregularities possibly could affect the waves more than the

electrons do. The measurements might then yield information

about the lunar surface or about the temporal and spatial variations of the cislunar medium. (Met. Abst. 11L-123. ) --Authors' abstract.

D-977 Fediakina, N. I. , Anomal'noe poqloshchenie v mae i iiule

1959 q. po nabliudeniiam v bukhte Tiksi metodom kosmicheskoqo radioizlucheniia. (Observations of abnormal absorption in May and July 1959 in Tiksi Bay with the method of

cosmic radio emission.) Akademiia Nauk SSSR. Mezhduvedomstvennyi Komitet po Provedeniiu MGG, Sbornik Statei V

Razdel Programmy MGG (Ionosfera ), No. 5:20-27, 1960.

3 figs. , table, 5 refs. English summary p. 26-27. DLC--

An abnormally high absorption observed in the Polar zone

during May and July of 1959 at a frequency of 32 MHz with

the method of the cosmic radio emission is described. Four

cases of such an absorption have been observed during the

period from Oct. 1, 1958 to Sept. 1, 1959. On all occasions

355
the absorption was preceded by a solar radio noise storm

which continued for 1. 5—5 hrs. Within 2—5 hrs after the

commencement of the solar radio noise storm there was

noted an increase of the absorption. The absorption increased for about 20 hrs and at a maximum it reached 9—11

db. The absorption decreased in the course of several days.

Within 20—40 hrs after the commencement of the solar radio

noise storm a magnetic storm began. During the storm the

absorption decreased rather than increased. The more intensive the magnetic storm, the sooner the absorption decrease occurred. Rapid absorption changes (as much as 3. 5

db per min ) during the magnetic storms on the 15, 17—19

of July, 1959, were observed. A supposition is made that

the abnormally high absorption is produced by corpuscular

particles ejected by the Sun during the strong chromospheric

flares of May 10 and July 9, 14 and 16. The velocities of

these particles considerably exceed the velocities of cor- puscular streams producing magnetic storms. --Author's abstract.

i . D-978 Fleischer, Robert (Rensselaer Poly. Inst., Troy, N. Y.),

Variations in 18 Mc/s solar and cosmic noise. (In: Paris

Symposium on Radio Astronomy, July-Aug. 1958, (Proceedings), pub. Stanford Univ. Press, 1959. p. 208-209. fig.,

3refs.) DLC (QB475. P26) -The apparatus for measuring

changes in the received intensity of 18 Mc/s cosmic noise

has been in operation at the Sampson Station of the Observatory of Rensselaer Polytechnic Institute since Feb. 1957.

The purpose of the apparatus is to record sudden cosmic

noise absorption (SCNA) as indirect indications of solar

flares, depending on the effect on the ionosphere of the ionizing radiation from the flares. The program is related to the

IGY. It is suggested that the bursts investigated are of

solar origin. It was found that in addition to the bursts that are specifically associated with flares, on days of general

solar disturbances, such as the Special World Intervals of

the IGY, there is a general "noisiness " or variability of the

18 Mc/s record. On such days it is very difficult to say

when the radiation is enhanced and when it is absorbed.

This mean level may be higher or lower, or the same, as on

more quiet days. Recorder tapes in pictorial form and other

patrol data will be published in a series entitled "Rensselaer

Observatory Publications »' --E. Z. S.

D-979 Ginzburg, V. L. (Lebedev Physics Inst. , Acad. Sci. , USSR ),

O neionosfernykh kolebaniiakh intensivnosti radioizlucheniia

tumannostei. (Non-ionospheric fluctuations in the intensity

of radio emission from nebulae. ) Akademiia Nauk SSSR,

Doklady, 109(l):61-63, July 1, 1956. 6refs.,4eqs. DLC--

356
It is generally accepted that fluctuation of the intensity

scintillation of discrete sources of cosmic clouds is caused

solely by earth's ionosphere. Thence, the recently established fact that these excited intensity fluctuations from

some source of non-ionospheric nebulae led to the assumption that this source is of stellar dimensions. Since evidence for non-ionospheric fluctuations are as yet inadequate,

the author examines the conclusions that would have to be

drawn should the existence of non-ionospheric scintillation

of discrete sources be established definitely. It is also

suggested that the source may not be stellar and the scintillation may depend upon the propagation of radio waves in

interstellar or interplanetary space. (Met. Abst. 9A-112. ) -I.L.D.

D-980 Gringauz, K.I. and Rudakov, V.A. , Measurements of elec - tron concentration in the ionosphere up to altitudes of 420-

470 km. carried out during the International Geophysical

Year by means of radio wave transmissions from the geophysical rockets of the Academy of Sciences, USSR. Planetary

and Space Science, N. Y. , 3(3/4): 133-193, Dec. 1961. 6

figs. , 18 refs. , 10 eqs. DWB. Transl. by R. Matthews of

original Russian, Ismereniia elektronnoi kontsentratsii v

ionosfere do vysot 420-470 km, provedennye vo vremia MGG

pri pomoshchi radiovoln, izluchavshikhsia s geofizicheskikh

raket AN SSSR in Iskusstvennye Sputniki Zemli, No. 6:48-32,

1961. DWB--Comparison of the sections of the curves relating electron concentration to altitude above the principal

ionization maximum (over 300 km), obtained from three rocket flights, indicates that the rate of electron concentration

decay with altitude over the one geographical location may

vary over a wide range (apparently according to time of year

and day), thus contradicting the earlier concept of an ionization model only slightly dependent on time of day, season,

latitude, etc. The variability in the fall-off rate of ionized

particles with altitude in the upper ionosphere v/as confirmed

by results obtained from ion traps installed on the third

Soviet earth satellite. The results confirm a principal electron concentration maximum in the ionosphere at altitudes

around 300 km and that the so-called E layer of the ionosphere

appears only as the result of the limited possibility of a purely altitude distribution of electron concentration on the basis

of the altitude -frequency characteristics obtained from ionosphere stations. An assessment of the possibilities of using

the dispersion interferometer at altitudes of some thousands

of kilometers indicates their unreliability, reaching impossibility at distances greater than 20, 000 km. --Authors' abstract.

357
D-981 Hanel, R.A. and Stroud, W. G. (both, Goddard Space

Flight Cen. , NASA, Wash. , D. C. ), The Tiros II radiation

experiment. Tellus, Stockholm, 13(4): 486-488, Nov. 1961.

7 figs. (incl. 5 color maps), table, 4 refs. DWB, DLC--

The Tiros II meteorological satellite, containing two television cameras and a family of electromagnetic radiation ex- periments, was placed into orbit on Nov. 23, 1960. The

medium resolution radiometer is a cluster of five sensors,

their optical axes inclined at 45 to the spin axis of the

satellite. The spin of TIROS provides the scanning motion.

Channels are sensitive to the following spectral bands:

(1) 6 to 6. 5; (2) 8 to 12; (3) 0. 2 to 6; (4) 8 to 30; and

0. 55 to 0. 75 microns. --Authors' abstract.

D-982 Harrower, G. A. , A consideration of radio star scintillations

as caused by interstellar particles entering the ionosphere . Pt. 1. Daily and seasonal variations of the scintillation of a radio star. Canadian Journal of Physics, Ottawa, 35(5):512-

521, May 1957. 6 figs. , 9 refs. Pt. 2. The accretion of

interstellar particles as a cause of radio star scintillations.

Ibid. , p. 522-535. 12 figs. , 2 refs. , eqs. Pt. 3, The kind,

number, and apparent radiant of the incoming particles. Ibid.

,

35(7): 792-798, July 1957. 2 figs. , 7 refs. DWB, DLC--In

Pt. 1, an analysis is made of measurements of the scintillations of the radio source in Cassiopeia recorded at Ottawa

during 1954 at a frequency of 50 Mc/s. After removal of the

effect of the altitude of the source, the data show certain

daily maxima occurring at solar times dependent on the date

of the year. These maxima are found to comprise five separate groupings, two being present roughly from Sept. 13 to

March 30, and the other three for the remainder of the year.

The obvious lack of circular symmetry suggests a cause external to the solar system, such as the infall of interstellar

particles. The apparent directions of arrival of these particles are derived from the scintillation measurements. In

Pt. 2, a previously reported analysis of measurements of

radio star scintillation, which showed daily variations dependent on time of year, is here interpreted to be the result

of the accretion of interstellar particles by the sun's gravitational field. After a brief general discussion of the accretion process, the measurements are examined in an attempt

to provide an explanation on that basis. Five distinct features exhibited by the scintillation data are interpreted as

resulting from particles arriving at the earth as follows:

directly from interstellar space, from a collision region behind the sun (both directly and after having crossed the

earth's orbit), and from the collision region by a process of

accretion in the gravitational field of the earth. The velocities of certain of these particles are derived by simple

358
applications of vector addition employing the known velocity

of the earth. The collision region is calculated to be located

a radial distance of 200 million miles from the sun. In Pts.

1 and 2, as the result of an analysis of measurements of the

scintillations of the radio source in Cassiopeia, it was suggested that interstellar particles, captured by the gravitational field of the sun, contributed to the observed features.

Arguments presented in Pt. 3 lead to the conclusion that

such particles must be hydrogen atoms. The number of hydrogen atoms reaching the earth is estimated to be 6 x 10^/m2/

sec. Their energy averages 9 or 22 electron volts, depending

on whether or not they are ionized. It is concluded that the

effect of this infall on the Earth's ionosphere would be more

than adequate to produce scintillations. The location of the

radiant, subject to the possibility of some considerable error,

is judged to be right ascension 17 hrs, declination -30 . Based on this position of the radiant, the velocity of the interstellar hydrogen atoms in the vicinity of the sun is found

to have the components: tangential 28 x 10^ rn/sec, radial

2 x lO^m/sec, and transverse 0. 2 x lO^m/sec, with respect

to the plane of our galaxy. (Met. Absts. 9A-152 and 9A-155)

--Author's abstracts.

D-933 Haslam, C.G.T. (Nuffield Radio Astron. Labs., Jodrell

Bank), An attempt to observe the occultation of a radio

source by Jupiter. Observator, London, 81(922): 108, June

1961. --The reason for failure in observing an occultation of a radio source by Jupiter on Oct. 23, 1960, was discussed.

The source of radio emission was evaluated at a few minutes

of arc. If the diameter were appreciably greater than 2'5,

no occultation by Jupiter could occur. Also, a probable

error in declination of the source is several times Jupiter's

angular diameter. --S. N.

D-984 Hoyle, F. and Narlikar, J.V. (both, St. John's College,

Cambridge), On the counting of radio sources in the steady

state cosmology. Royal Astronomical Society, London,

Monthly Notices, 123(2): 133- 166, 1961. 7 figs. , 2 tables,

16 refs. , 36 eqs. DLC--The problem of the number count of

radio sources as a function of the incident flux is shown to

depend on two crucial features: (i) the size and behavior of

condensations; (ii) the dependence on age of the probability

of a galaxy being a radio source. Provided the probability

rises by a factor 10^ for galaxies with ages from H-l to

about 2. 5"1, and provided the primary condensations of the

steady-state theory possess initial dimensions of order 30

megaparsecs, the radio source count can rise more steeply

than is the case for sources uniformly distributed in Euclidean space. Each primary condensation contains of the order

359
5

of 10 galaxies, which in the main expand apart from each

other as the universe expands. It is shown that a luminosity function can be chosen for the radio sources giving re- sults consistent with observation, not only for the source

count, but also with the data on angular diameters and with

experience in the problem of optical identifications. --Authors' abstract.

D-9S5 Istomin, V. G. , Variation in the positive ion concentration

with altitude from data of mass spectrometry measurements

on the third satellite . Planetary and Space Science, N. Y. , 8(3/4): 179-182, Dec. 1961. fig., 7 refs. , eq. DWB.

Transl. by R. Matthews of original Russian, Ismenenie

kontsentratsii polozhitel'nykh ionov s vysotoi po dannym

mass-spektrometricheskikh izmersnii na tret 'em sputnike,

in Iskusstvennye Sputniki Zemli, No. 8, p. 127-131, 1961.

DWB--Up to altitudes of 550 km the variation in positive ion

concentration is in satisfactory agreement with the variation

in electron concentration, while above 650 km mass spectrometry measurements, show a wide diversity on three different days. A comparison of mean concentration measurements obtained by mass spectrometry with experimental data

employing ion traps provides conformation of the O concentration as a function of altitude, and of electron concentration as a function of altitude. The agreement between the N,

O, NO and O positive ion concentration against altitude and

the electron concentration curve points to the fact that light

ions, with mass numbers beyond the range of the instrument

(hydrogen ions H, and H, and helium He ) do not exist in

appreciable quantities and the ionosphere up to 900 km re- mains oxygen -nitrogen. With the presence of light ions, it is natural to expect an increase in their relative concentrations with altitude, as is found for ions of atomic nitrogen

in relation to ions of atomic oxygen and for ions of atomic

oxygen in relation to still heavier ions/1, 2/. An increase

in relative concentrations of ions H, H and He would thus

lead to a divergence between the electron concentration and

the ion concentration. --Author's abstract.

D-986 Kallmann, H. K. (Rand Corp. , Santa Monica, Calif. ),

Variable atmospheric properties derived from rocket and satellite observations. Journal of Atmospheric and Terrestrial

Physics, London, 23:330-337, Dec. 1961. 3 figs. , 2 tables,

26 refs. , 4 eqs. DLC--Upper air densities obtained by means

of rockets and satellites in the region from 100 km to about

800 km are presented. Variations of densities from day to

night become apparent around 200 + 30 km; the effect increases with altitude. Pressures and scale heights are derived from densities, and preliminary mean values for day and

360
night are obtained. From the variation of scale height with

altitude, regions of constant temperature and of variable

molecular weight have been determined. It has been found

that the mean temperature at 300 + 50 km is approximately

1400 K. Shortly after midnight, the temperature drops to

about 1010 K, and stays approximately constant above 150

+ 10 km. --Author's abstract.

D-S87 Kornesaroff, M. M. (C.S. I. R.O. , University Grounds,

Chippendale, N. S. W. ), Galactic radio spectrum down to

19. 7 Mc/s. Australian Journal of Physics, Melbourne,

14(4):515-52S, Dec. 1981. 4 figs. , 3 tables, 14 refs.

13 eqs. DLC--Studies of the galactic radio spectrum have

been carried out using results of a number of surveys between 19. 7 and 1390 Mc/s. About 4-5 from the equator

the spectrum is non-thermal and the temperature spectral

index has a constant value of 2. 3 + 0. 1. The form of the

spectrum changes with decreasing latitude, and at the lowest frequency an intensity minimum is observed along the

equator. It is shown that the observations are fully consistent with a model consisting of two components: (i) nonthermal sources of constant spectral index, (ii) ionized

hydrogen of constant temperature. The results yield some

information about the distribution of thermal and non-thermal

emissivity in the galactic plane, and provide qualitative support for results which Westerhout has drawn from more limited spectral data. --Author's abstract.

D-988 Kuz'min, A. D. , O diskretnom istochnike radioizlucheniia

& = 18 53 .7; O - 1 13'. (Discrete source of radio emission OL = 18 531 .7, O - 1 13'.) Astronomicheskii Zhurnal,

Moscow, 38(5):905-911, Sept. /Oct. 1931. 3 figs. , table,

22 refs. , 3 eqs. Russian and English summaries p. 905.

Transl. into English in Soviet Astronomy AJ, N. Y. , 5(5):

692-393, March/April 1962. DLC--Results of the study of

the discrete source of radio emission 0t= 18 53* . 7, o

~

1 IS', are given. The observations were made at 9.3 cm

v?ith the 22 meter radio telescope of the Physical Institute of

the USSR Academy of Sciences. The flux density of radio

emission and the angular dimensions of the source are determined. The derived data are compared with those of other

authors. The spectrum of the source is obtained; it is nonthermal. The spectral index 0. 4 + 0. 1 is derived. Shklovsky's method is used for the determination of the distance to

the source, R=3500 pc. The radius of the source at this

distance is r-9 pc. The minimum total energy of relativistic

particles and the magnetic field, within the source, is found

331
50

to be 10 ergs. The magnetic field strength in the source

.4 H - 10 gausses. A comparison is made with the discrete

radio source, identified with the nebula IC 443. The spectrum of this source is obtained. The spectral index is 0. 5 +

0. 1. The similarity of the compared sources as regards to

structure, spectrum, dimension, total energy and field

strength is shown. On the basis of the above and also the

large value of the energy, within the nebula, it is concluded

that the studied source is a remnant of a type II supernova.

The erroneous results obtained by Pari j sky, assuming a thermal radiative mechanism, are noted. --Author's abstract.

D-989 Large, M.I. ; Mathewson, D. S. and Haslam, C.G.T. (all,

Nuffield Radio Astronomy Labs. , Jodrell Bank), Radio sur- vey of the galactic plane at a frequency of 408 Mc/s, Pt. 1,

Discrete sources. Royal Astronomical Society, London,

Monthly Notices, 123(2): 113-122, 1961. 4 figs. , table, 28

refs. Pt. 2, Continuum emission from the galactic disk,

p. 123-132. 5 figs. , 12 refs. , 2 eqs. DLC--Part of the

galactic plane has been surveyed at 408 Mc/s using the 250

ft radio telescope at Jodrell Bank. The results are compared

with the Sydney 85 Mc/s survey and the Leiden 1390 Mc/s

survey in order to group the discrete sources of radio emission according to their spectral index. Of 51 sources, 36

are found to have a spectral index consistent with the as- sumption that they radiate thermally, and 15, including the

source at the galactic center, have a non-thermal spectral

index. Most of the sources lie within 1/4 of the new galactic plane, and are thought to be at distances of several

kiloparsecs. Some of the thermal sources are a few degrees

from the galactic plane, and probably less than one kiloparsec from the Sun. The continuum background emission from

the galactic disk is discussed in a second paper. The 408

Mc/s Jodrell Bank survey of the galactic plane has been used

in conjunction with the Sydney (85 Mc/s) survey and the

Leiden (1390 Mc/s) survey to delineate the distribution of

thermal and non-thermal radio emission from the Milky Way.

The results of this analysis are presented in the form of both

isophotes and profiles at constant galactic latitudes. They

extend and confirm a similar analysis carried out by Westerhout. Some features of the distributions could indicate a

spiral structure of the Galaxy, but it is found that there are

difficulties in fitting Mill's spiral model to the parts of the

Milky Way ween from the northern hemisphere. --Authors'

abstract.

362
D-990 Leinbach, H. and Reid, G. C. (both. College, Alaska),

V. H. F. radio wave absorption in northern latitudes and solar

particle emissions . (In: International Scientific Radio Union.

IGY Committee, Some ionospheric results obtained during the

IGY. Amsterdam, Elsevier, 1961. p. 281-294. 2 figs.

,

table, 32refs.) DLC (QC879.I68), DWB (M10. 535 I612so)

--Extensive observations of the absorption of radiowaves as- sociated with ionospheric disturbances have been obtained at

high latitudes by using the cosmic noise technique. The high

latitude ionospheric absorptions were divided into three types:

Type I as a SID accompanying a solar flare; Type III following the flare as a strong slowly varying absorption persisting

for 45 hrs. After 46 hrs the absorption shows rapid variations

of Type II coinciding with auroral and magnetic activities. The

characteristics of Type III are described in detail and tabulated for the period of July 3 to Sept. 22, 1957. The Type III absorption due to ionization caused by high energy protons is

atmospheric in origin, the result of attachment of electrons

to form negative ions during the night and photo-detachment

of the same electrons during the daytime. The proton energy

is evaluated to 8 Mev and the penetration into the atmosphere

to a height of 67 km. The interplanetary density of the fast

protons is probably very low. The state of the interplanetary

medium may be revealed by the Type III absorption. (Met.

Abst. 13F-133.)-S.N.

D-991 Liszka, L. (Kiurna Geophysical Obs. , Sweden), Local

electron densities deduced from the Faraday fading of satellite transmissions using measurements during two consecutive transits. Planetary and Space Science, N. Y. , 5(3):213-

219, July 1961. 5 figs. , 4 refs. , 30 eqs. DWB--A simplified method for analysis of the Faraday fading measurements

is described. With a satellite of circular orbits, both the

total electron content between observer and satellite and the

direction of the magnetic field in the ionosphere can be calculated. For all other orbits the local electron density must

be taken into consideration. From measurements of the Faraday fading frequency during at least two consecutive transits

the total electron content and the local electron density can

be calculated as a function of satellite altitude on the following assumptions: (a) during the period of time comprising

two consecutive transits the relative gradients of local electron density are constant at the same altitudes; (b) the local

electron density at altitudes above the F2 maximum during a period of time comprising two consecutive transits changes

as does the electron density within the maximum of the F2

layer. The method has been applied to the daytime observations of the 1958 S 2 on Sept. 12 and 29, 1959. --Author's

abstract.

353
D-992 McLean, D.J. and Wild, LP. (both, C.S.I. R.O., Univ.

Grounds, Chippendale, N. S. W. ), Systems for simultaneous

image formation with radio telescopes . Australian Journal of

Physics, Melbourne, 14(4):489-496, Dec. 1961. 5 figs. , 3

refs. , eq. DLC--The large arrays of aerials often necessary

for high resolution in radio astronomy are generally used to

observe a brightness distribution in an area of the sky by

scanning the aerial beam, point by point, across the area.

In this paper we investigate the possibility of observing the

complete distribution simultaneously over a given area. Two

possible analogue systems capable in principle of forming

such images, are described: in one, the analogue image is

formed optically, in the other with ultrasonic methods. The

problems and limitations of the two systems are examined

and it is concluded that further technical developments are required before practical systems with useful sensitivity and

resolution can be achieved. --Authors' abstract.

D-993 Miller, Raymond J. (General Electric Co. , Ithaca, N. Y.),

Air and space navigation system uses cross correlation detection techniques . Electronics, N. Y. , 34(50):55-59, Dec.

15, 1961. 6 figs. , ref. , eq. DWB, DLC-The correlation

navigator is a self contained surface speed and drift angle

measuring system, which, unlike Doppler systems, takes

advantage of unique characteristics of radar signal returns

from individual scatters. It measures altitude above any

terrain, regardless of its nature or state, and renders the

surface speed of aircrafts or space vehicles. The cross

correlation detection technique and other features are described in some detail. (Met. Abst. unpub. )--W. N.

D-994 Millman, George H. ; Sanders, Armand E. and Mather,

Robert A. , Radar - lunar investigations at low geomagnetic

latitude . Journal of Geophysical Research, Wash., D. C. , 65(9):2619-2626, Sept. 1960. 8 figs. , 10 refs. , 6 eqs.

DLC--Radar reflections from the Moon have been studied

utilizing the Trinidad, BWI, radar operating in the 400 Mc/s

frequency range. The Moon has been tracked from moon rise

through transit during periods of sunset. On all occasions,

the rotation of the plane of polarization (Faraday effect) was

observed. Absolute values of the total electron content of

the ionosphere deduced from these measurements and the

electron content above the height of the F layer maximum,

evaluated from vertical incidence ionospheric soundings re- corded at the NBS Puerto Rican station, are presented. (Met.

Abst. 13F-157.) -Authors' abstract.

364
D-995 Mills, B. Y. ; Slee, O. B. and Hill, E. R. , Catalogue of

radio sources between declinations -50 and -80 . Australian Journal of Physics, Melbourne, 14(4):497-507, Dec.

1961. 5 tables, 15 refs. DLC--A catalogue has been prepared of the radio sources observed between declinations

-50 and -80 , using the Sydney cross type radio telescope

at a wavelength of 3. 5 m; a total of 219 sources is listed.

This supplements the earlier catalogues for the declination

ranges + 10° to -20° and -20° to -50°. In addition to the

positions and intensities of the sources, angular sizes of

42 of the strongest sources are given. As before, identifications with bright optical objects have been sought, and

a number of possible identifications with emission nebulae

and bright galaxies are listed. Because of the small area

of sky covered by the present catalogue, the numbers of

sources are small (compared with those in our earlier catalogues ) so that the statistical analysis of their distribution

has comparatively low weight. However, the analysis

gives results consistent with those obtained using the earlier catalogues. Finally, the present state of the identification of sources in our catalogues is briefly reviewed. -- Authors' abstract.

D-996 Mitra, A. P. and Sarada, K. A. (both, Nat'l. Physical Lab.,

New Delhi, India ), Determination of the electron content

of the outer ionosphere from measurements of cosmic radio

noise absorption. Journal of Atmospheric and Terrestrial

Physics, London, 23:348-357, Dec. 1961. 5 figs. , 3 tables,

11 refs. , 9 eqs. DLC --Simultaneous use of ionograms and

observations of cosmic radio noise taken at New Delhi (at

22. 4 Mc/s ) have yielded approximate values of the electron

content of the outer ionosphere. It has been assumed that

the electron density falls out exponentially from the level of

maximum ionization. The value of the exponent was determined to be about 6 x 10'3/km. --Authors' abstract.

D-997 Molchanov, A. P. , Spektr lokal'nykh istochnikov radioizlucheniia Solntsa. (The spectrum of local sources of solar

radio emission. ) Astronomicheskii Zhurnal, Moscow, 38(5):

849-854, Sept. /Oct. 1961. 3 figs. , 20 refs. , 3 eqs. Russian and English summaries p. 849. Transl. into English in

Soviet Astronomy AJ, N. Y. , 5(5):551-354, March/April 1932.

DLC --The relative spectrum of a source on the Sun, observed

during a solar eclipse, has been obtained. The mean inclination of the spectra is determined from measurements of the

maximum shift of the center of gravity of solar radio emission.

The absolute spectrum is computed, adopting several assumptions on the dependence between the emission flux of a quiet

Sun and the wave length. The magnetic field in the source is

385
found from the inclination of the spectrum. A conclusion is

made on the necessity of assuming either the presence of

strong magnetic fields in the sources or the existence of a component of non-thermal emission. --Author's abstract.

D-998 Naismith, R. and Smith, P. A. (both, D. S. I. R. Radio Res.

Station, Slough, Bucks), Further evidence of a long term

variation in the relationship of solar activity to the ionosphere. Journal of Atmospheric and Terrestrial Physics, London, 22(4): 270-274, Dec. 1961. 4 figs. , table, 2 refs.

DLC --Ionospheric measurements indicate that during the last

20 yrs there has been a progressive decrease in F region

ionization corresponding to a given sunspot number. In a previous paper it was shown that there was a corresponding

decrease in the E region. It is pointed out that this represents a progressive change in the nature of solar radiation

or in the atmosphere. --Authors' abstract.

D-999 Noton, A.R.Maxwell (Elec. Eng. Dept. , Univ. Nottingham),

Guidance of space vehicles by radio measurements and command. British Interplanetary Society, Journal, 18(4): 132-138,

July/Aug. 1961. 4 figs. , table, 2 refs. , 13 eqs. DWB, DLC

--The injection of space vehicles into orbit is dependent on

guidance and control systems which are effective during the

powered flight in the vicinity of the Earth. However, for

most advanced lunar or interplanetary missions, the injection will not be sufficiently accurate and forms of post injection guidance will be employed. This paper is concerned

with such guidance and in particular with the important radio

command system which depends on ground radio tracking,

computing and command. After summarizing the necessary

ballistics theory, schemes of mechanization are discussed

assuming the use of a small rocket (chemical propellant)

mounted in the space vehicle. The computation of the midcourse correction depends on the orbit determination, based

on radio tracking of the vehicle by several sites located at

widely dispersed points on the surface of the Earth. The

method of orbit determination is explained and finally, for

lunar and interplanetary missions, some examples are given

in which the overall accuracy of such guidance systems has

been calculated in terms of the various sources of error,

e. g. , in pointing the rocket and determining the orbit from

noisy radar data. --Author's abstract.

363
D-1000 Pariiskii, Iu. N. , Model' tumannosti Oriona po radionabliudeniiam. (Model of the Orion nebula from radio observations. ) Astronomicheskii Zhurnal, Moscow, 38(5): 798-808,

Sept. /Oct. 1961. 10 figs. , table, 39 refs. , 4 eqs. Russian

and English summaries p. 798. Transl. into English in

Soviet Astronomy AJ, N. Y. , 5(5):611-618, March/April 1932.

DLC--The coordinates and radio brightness distribution of the

Orion nebula have been obtained with the Pulkovo large radio

telescope. A comparison with previously measured coordinates of the radio source shows that the maximum of radio

emission coincides with the position of the Orion trapezium.

The kinetic temperature of the nebula is derived from the distribution of radio brightness at 8. 3 cm. A method for determining the kinetic temperatures of gas nebulae of arbitrary

structure is described, it being a generalization of Wade's

method. The value of Te = 11750 K obtained from radio data

is close to that found from optical observations. The mean

square electron density in the nebula differs considerably

from the electron density derived from the relative intensities

of the lines 3726/3729, the difference increasing with the

distance from the trapezium. If this difference is interpreted

as a result of the cloud structure of the nebula, the fraction

of the volume occupied by dense clouds is 1/14 in the center

and exceeds 1/36 at the periphery of the nebula. The mass

of the nebula is found to be 116 Mq, about 6 Mq being concentrated in its brightest part having a diameter of 3'. The

emission measure obtained from radio observations is essentially smaller than that predicted from the brightness of the

nebula in H/# . It is possible that the "excess" emission in

H/3 is connected with the existence of separate very hot formations, in which excitation due to hydrogen collisions becomes essential. Such formations can exist as a result of

the presence of a system of shock waves in the nebula during

its expansion. --Author's abstract.

D-1001 Payne-Scott, Ruby and McCready, L.L., Ionospheric effects

observed during dawn observations on solar noise. Journal of

Geophysical Research, 53(4):429-432, Dec. 1948. -Near

dawn measured interference pattern of direct radiation from

the sun, combined with reflected energy from the sea. Both

60 and 200 Mc/s were used. Found the refractive effects

about three times as great as would be produced by a symmetrical parabolic F layer with constants similar to the lower

side. (Unchecked )--L. A. Manning

367
D-1002 Pawsey, J. L. , Radio star scintillations due to ionospheric

focusing. (In: Physical Society, London, Physics of the

Ionosphere. London, Physical Society, 1955. p. 172-173.

)

DWB--A new type of scintillation of the radio star in Cygnus

has been detected which cannot be attributed to scattering

from a number of randomly distributed ionospheric irregularities, but appears to be due to a focusing effect of lens-like

irregularities. The irregularities are elongated in directions

which vary from time to time, and it is not yet possible to

decide in which part of the ionosphere they exist. (Met.

Abst. 13F-174.) -Physics Abstract 8423, 1955.

D-1003 Pineo, V.C. and Briscoe, H. W. (both, Lincoln Lab. , Mass.

Inst, of Techn. ), Discussion of incoherent backscatter

power measurements at 440 Mc/s. Journal of Geophysical

Research, Wash., D. C. , 68(ll):3955-3963, Nov. 1951.

9 refs. , 4 eqs. DWB, DLC--The Mill Stone Hill backscatter

power measurements were improved by taking into account

certain approximations. The observed scattered power was

compared with GORDON'S (1958) original prediction which

was based on independent scattering by free electrons.

More recently developed theories (FEJER, 1960; DOUGHERTY

and FARLEY (1960) show that at radio wavelengths greater

than the Debye length, the electrons do not behave independently of each other, and that the scattered power is approximately one half what it would be for free electrons. Hence,

the scattered power measurements at 440 Mc were about 7 db

less than Gordon's prediction and 4 db less than predictions

based on latest theories of electron scattering. --S.N.

D-1004 Ponomarev, E. A. , Nekotorye voprosy rasprostraneniia

kolebanii nizkoi chastoty v viazkoi i szhimaemoi plazme

vdol' magnitnogo polia. (Some problems on the propagation

of low frequency oscillations in a viscous compressible

plasma along the magnetic field. ) Astronomicheskii Zhurnal,

Moscow, 38(5):877-884, Sept. /Oct. 19S1. 8 refs. , 47 eqs.

Russian and English summaries p. 877. Transl. into English

in Soviet Astronomy AJ, N. Y. , 5(5):673-377, March/April

1962. DLC --The" propagation of low frequency electromagnetic, transversal viscous and longitudinal oscillations in

plasma along the magnetic field, is considered. Relations

are obtained, which generalize the known magneto-hydrodynamic equations for the case of higher frequencies. The

connection between the electric conductivity and viscosity

coefficients is given. The energy exchange between different forms of waves is considered. Qualitative estimates,

applicable to conditions in the solar corona, are made.

--Author's abstract.

338
D-1005 Ratcliffe, J. A. (Cambridge, Great Britain), S. I. D. 's during the IGY . (In: International Scientific Radio Union.

IGY Committee, Some ionospheric results obtained during

the IGY. Amsterdam, Elsevier, 19S1. p. 124-129. 4 figs.,

6 refs. , 3 eqs. French summary p. 129. ) DLC (QC879.

168), DWB (M10. 535 I612so) -Measurements of the

changes of phase and amplitude of waves reflected from the

E layer on frequencies of 2. 4 and 2. 8 Mc/s and from the

F layer on frequencies of 4 and 6 Mc/s and changes of amplitude of waves emitted from radio stars on frequencies of

16 and 24 Mc/s, were all carried out simultaneously during

the course of a S. I. D. The results from about 50 S. I. D. 's are discussed. It is suggested that they provide reason

for supposing that extra electrons are produced during an

S. I. D. , at all levels between about SO km and 120 km and

that the distribution changes from one S. I. D. to another.

This suggestion is shown to be compatible with evidence

from experiments of different kinds. (Met. Abst. 13F-187.

)

--Author's abstract.

D-1006 Rutherford, G.T. (Bureau of Met. , Melbourne), Review of

the application of satellites to meteorology. Australian

Meteorological Magazine, Melbourne, No. 34:1-14, Sept.

1961. 3 figs. , 11 refs. DWB--The increase in meteorological knowledge during the past half century has not been ac- companied by a parallel increase in accuracy of forecasts.

This has been due, not only to a continuing absence of information from certain vital areas, but also to a more fundamental and scientific difficulty of inadequate understanding

of meteorological processes, necessitating reliance on empirical and largely subjective forecasting techniques. In

this paper reference is made to the potential of the weather

satellite, by television camera and radiation sensor, to re- move the former of these limitations by extending the field

of observation from the present one -quarter of the Earth's

surface to the entire globe. The importance of radiation

measurements by satellite sensors for extended range forecasting by heat balance considerations is also discussed

together with other applications of these measurements. It is concluded that while availability of observations on a global basis from weather satellites will be a major advance,

it will not prove a panacea for all meteorological ills. The

additional requirement is a better understanding of meteorological processes. This is still a long term prospect but close

study and interpretation of photographed cloud patterns is

one avenue which promises to lead to this result and consequently to better weather prediction. --Author's abstract.

35S
D-1007 Shain, C.A. ; Komesaroff, M. M. and Higgins, C.S.

,

High resolution galactic survey at 19. 7 Mc/s. Australian

Journal of Physics, Melbourne, 14(4):508-514, Dec. 1961.

Graph (fold), 14 refs. DLC--An extensive strip of the

Southern Milky Way has been surveyed at 19. 7 Mc/s, using

a Mills Cross with a pencil beam 1. 4 wide. The radio contours show a number of dark areas whose positions agree

with those of optically observed H II regions which at this

frequency are seen in absorption. In addition, an intensity

minimum along the galactic equator appears to represent the

effect of absorption due to many H II regions extending to

great distances in the galactic plane. --Authors' abstract.

D-1008 Swift, D. W. (AVCO Corp. , Wilmington, Mass. ), Effect of

solar X-rays on the ionosphere. Journal of Atmospheric and

Terrestrial Physics, London, 23:29-56, Dec. 1961. 15 figs.,

3 tables, 20 refs. , 39 eqs. DLC--Quite often a large solar

flare is accompanied by a Sudden Ionospheric Disturbance

(SID) in which the electron density of the D region undergoes a rapid increase in a matter of minutes. There is strong

evidence that the rapid increase is caused by soft X-rays generated in the Sun's corona during a solar flare. The X-rays

reach the D region where they are capable of producing ionization. Extensive computations have been carried out in

order to understand the effects caused by a burst of solar Xrays in the D region. In general, the altitudes for peak production range from 95 km for 1 keV X-rays down to 60 km for

9 keV X-rays. The rate equations are set up (and solved,

with the aid of an IBM 704 computer), assuming several

specific energy distributions and a duration of 6 min for a solar flare. The various processes are also studied separately by solving the rate equations under simplifying assumptions. The assumption of a detailed electron negative ion

balance led to results which agreed very well numerically

with those obtained by machine computations. It is found

that the maximum relaxation time for equilibrium between

the electrons and negative ions is about 2 sec. Since re- combination times are at least two orders of magnitude longer

than the relaxation time for equilibrium between the electron

and negative ions, a detailed electron-negative ion balance

will hold at all altitudes in the D region throughout an SID.

The number of free electrons decreases with increasing Xray energy. This is because the higher energy X-rays deposit most of the ionization at the lower altitudes where the

electron attachment rate is much larger than the detachment

rate. Therefore, most of the ionizing radiations will then go

over to the production of negative ions. Also, recent solar

X-rays measurements are discussed and used for computing

electron densities. Finally, the computed electron distributions are compared with data deduced from ionospheric measurements. --Author's abstract.

370
D-1009 U. S. Weather Bureau, Catalogue of meteorological satellite

data; Tiros I television cloud photography. Its Key to Meteorological Records Documentation, No. 5. 31, 1961. 147 p.

mostly maps and tables. DWB--The Catalogue attempts to

provide information to research personnel making use of climatological data. It consists of a complete listing of cloud

photographs by Tiros I and a set of maps showing their geographical coverage. The tabulated listings give descriptive

information about the pictures obtained by Tiros I. Following the listings is a series of maps which provide a rough

indication of the area covered. A report by the Meteorological Satellite Laboratory describes the problems and uncertainties in specifying the satellite's attitude as a function

of time. --S. N.

D-1010 Vestine, E. H. , Physics of solar terrestrial space: lunar

flight. Rand Corp. , Santa Monica, Calif. , Paper 1344,

Feb. 24, 1958. 17 p. 3 figs. , 14 refs. DWB (M(055)

R186p)--This lecture discusses physical conditions in space

near the earth, moon, and sun. In particular, it deals with

density, radiation, temperature, wave propagation, magnetic

fields, and the effects of these factors on space flights.

--Author's abstract.

D-1011 Warwick, J. W. (High Altitude Obs. , Univ. of Colorado,

Boulder), Relation of Jupiter's radio emission at long wavelengths to solar activity. Science, Wash. , D. C. , 132

(3435): 1250-1251, Oct. 28, 1960. 2 figs. DLC--Since the

spring of 1960 a strong positive correlation between Jupiter's

decametric emission and solar decametric continuum emission observed at Boulder has been evident. The time delay

of 1 to 2 days, with solar emission preceding Jupiter's emission, suggests that fast solar corpuscles, at velocities of

the order of 0. 1 c, are directly involved in the planet's atmosphere or magnetic field. --Author's abstract.

D-1012 Watkins, CD. (Nuffield Radio Astronomy Lab. , Jodrell

Bank, Manchester Univ. ), The magnetic storm time variation of radio star scintillations and auroral radio echoes . Journal of Atmospheric and Terrestrial Physics, London,

19(3/4): 289-292, Dec. 1960. 3 figs. , 3 refs. DWB--An

examination of the observations made at Jodrell Bank during

1955-1958 shows that about 80% of all the series of radio

echoes recorded were preceded by a sudden commencement.

This suggests that echo activity is mainly related to s. c. type magnetic storms. The storm time variations of echo

incidence and mean scintillation rate are graphically presented. The variation of echo incidence is also plotted for

371
the periods Jan. 1955-June 1957 and July 1957-Dec. 1958

separately and combined, and the associated features are discussed. (Met. Abst. 13B-165. )«I. S.

ANONYMOUS

D-1013 Powerful VHF radar probes sun's corona. Electronics, N. Y. , 34(52):54, 56, Dec. 29, 1961. photo. DWB, DLC--Reports

on a long term study of radar echoes from the sun being conducted by the Lincoln Laboratory of MIT with joint U. S. Army,

Navy and Air Force support. The detailed study covers 32

radar measurements made during April 19 to July 7 near El

Campo, Tex. The findings are compared with those obtained

by Stanford in April 1959. Long term radar observations are stated to be capable of yielding quantitative data on the effective size and shape of the corona and other phenomena.

The characteristics and capabilities of the radar transmitter

operating with a 38. 25 Mc transmitting frequency is discussed. A photograph is presented of the half megawatt

radar and 1, 024 dipole antenna array used in gathering data

about solar phenomena. --D. B. K.

372
AUTHOR INDEX

Aarons, Jules D-l-7, 268, 489,

524, 895, 970

Acton, Loren W. D-8

Adgie, R.L. D-608

Agy, Vaughn D-730

Aitchison, G.J. D-9

Alaska. University. Geophysical

Institute D-10

Alekseev, U. D-S08

Allcock, G. McK. D-ll-14, 959

Allen, C.W. D-15, 215, 419

Allen, R. D-5

Al'pert, Ia.L. D-16-21

Alsop, L. D-249, 608

American Geophysical Union

Special Comm. on Cosmic

Terr. Relationships

D-22, 23

Anderson, D. S. D-24

Anderson, Lloyd J. D-25

Anderson, Roy E. D-26

Andre", Pierre D-27

Andrillat, Henri D-28

Appleton, Sir Edward D-29-34

Arendt, P. R. D-322

Archer, S. D-608

Armier, G. D-35

Aschenbrand, L. M. D-494

Astronomical Society of the

Pacific D-36

Athay, R. G. D-508

Australia. Commonwealth Scientific and Industrial Research Organization. Div.

of Radiophysics D-960

Avignon, Yvette D-37-39, 608

Bachynski, M.P. D-748

Bailey, Dana K. D-575

Bailey, V.A. D-40

Bain, W.C. D-41-43, 961

Baldinger, E. D-44

Baldwin, J.E. D-608

Banerjee, D. K. D-45

Banerjee, P. C. D-46

Banerjee, S. S. D-46, 47

Barron, William R. D-2, 3

Bartels, G. D-436

Barthle, R.C. D-976

Basinski, Jane D-808

Basler, Roy P. D-48

Basu, S. D-4

Bates, D. R. D-668

Bauer, Siegfried J. D-49, 158-

160, 962

Bazzard, G. H. D-50, 537,

538, 540

Beckmann, B. D-51

Becker, W. D-963

Beer, Arthur D-52, 213

Behr, A. D-53

Beliaev, N. A. D-54

Belrose, J. S. D-151

Bennewitz, Hans Gerhard

D-644

Benson, Robert F. D-964

Beringer, Robert D-181

Berkner, Lloyd V. D-55-57,

225, 575

Berry, J. W. D-151

Bertrand, Maurice D-164

Beynon, W. J. G. D-34, 58,

214, 226

Bhargava, B.N. D-965

Bhonsle, R. V. D-59, 60,

652-854

Bierman, L. D-81

Blackband, W. T. D-62, 63

Blauw, A. D-808

Bleeker,^ W. D-578

Blum, Emile-Jacques D-84-36,

608

Boischot, A. D-37, 67, 608

Bok, Bart J. D-68, 608

Bollhagen, H. D-772

373
Bolton, J. G. D-575, 611, 966

Booker, Henry G. D-69-74,

668

Bordovskii, G. A. D-404

Bost, R. D-75

Bournazel, J. D-6

Bowhill, S.A. D-517

Bowles, Kenneth L. D-76

Bowman, G.G. D-77

Boyd, R.L.F. D-502, 503

Bracewell, Ronald N. D-78-83,

524, 612

Braude, S. la. D-967

Bray, D. W. D-689

Bremmer, H. D-84

Brenan, I.N. D-85

Brenan, P.M. D-86

Briggs, B.H. D-87, 88, 575,

968

Briscoe, H. W. D-1003

Brito-Infante, Jose M. D-89

Brockman, James D-91

Brockman, M.H. D-91

Brown, G. M. D-58, 214, 226

Brown, Robert Hanbury D-92,

93, 608, 611

Brown, S. B. D-94

Bruce, G. E. R. D-95

Bruton, R.H. D-913

Bruzek, A. D-96

Buchanan, H. R. D-90

Buck, Richard F. "D-969

Budden, K.C. D-97, 98

Bugnolo, Dimitri S. D-99

Burbidge, E. Margaret D-608

Burbidge, G. R. D-608

Bureau, Robert D-100, 164

Burgess, B. D-63

Burgess, R. E. D-101

Burkard, O. D-102

Burke, B.F. D-229, 524

Burrows, Charles R. D-103

Cahill, W.F. D-282

Cain, J. C. D-104

Campbell, W.H. D-838

Caplan, P.J. D-826, .827

Carnegie Institution of Washington

D-105, 106

Carpenter, Martha (Stahr) D-107,

108

Carr, T. D. D-770, 772

Carru, H. D-109

Cartwright, D. G. D-206, 207

Casey, Joseph D-970

Castelli, John P. D-3, 7, 970

Chapman, J. H. D-110, 971

Chapman, Sydney D-lll, 668

Chatterton, N. D-772

Chechik, P.O. D-114

Chen, Fan-Yun- D-608

Chestnov, F.I. D-115

Chikachev, B. M. D-651

Child, C.H. D-116

Chivers, H. J. A. D-117-122

Choate, R.L. D-90

Chojkova' Eliska D-128-131

Christiansen, W.N. D-123,

124, 608

Chubb, T.A. D-125-127, 232

Chudesenko, E. F. D-17

Clegg, J. A. D-475

Coates, G.P. D-132

Coates, Robert J. D-133-135

Cocconi, Giuseppe D-136

Cognard, Rene D-468

Cohen, Marshall H. D-137-139,

608

Coleman, P. J. , Jr. D-695

Collins, C. D-682

Conway, R. G. D-972

Copeland, J. D-892

Corcuff, Y. D-140

Cornell University, Ithaca. School

of Engineering D-141, 142

Cottony, H. V. D-143

Coupiac, Pierre D-848

Coutrez, Raymond D-144, 294

Covington, Arthur E. D-145-149,

518, 608

Cowling, T. G. D-419

Cox, H. W. D-150

Craig, K.J. D-575, 608, 913

Crain, CM. D-804

Cranshaw, T. E. D-151

374
Crary, J.H. D-152

Crawford, Arthur B. D-575

Croft, T. A. D-153

Crone, W. Reed D-410, 412

Dumont, Rene D-194

Dungey, J. W. D-195

Dyce, R.B. D-196, 197, 348,

445

Dagg, M. D-154-157, 511,

973

Daniels, Fred B. D-49, 158-

161, 962

Danilin, B. S. D-499

Das, A.K. D-162, 163

Datta, S. D-711

Dauvillier, Alexandre D-164

Davies, J. G. D-165

Davies, Kenneth D-166

Davies, Rodney Deane D-167,

163, 608

Davis, Robert J. D-890

Davrton, D.I. D-188

Degaonkar, S.S. D-654

De Feiter, L. D. D-169, 226

de Groot, T. D-170, 171, 608

de Jager, C. D-608

Dellinger, John Howard D-172-

174

De Mastus, Howard D-175

de Mendonca, F. D-176

de Munck, J. C. D-226

Denisse, J. F. D-65, 66, 177-

179, 422, 608

Devenport, M.H. D-151

De Voogt, A. H. D-578

de Witt, J.H. D-180

Dewhirst, D. W. D-608

Dicke, Robert H. D-181

Dieminger, Walter D-182

Dinger, Harold E. D-183, 570

Dobriakova, F. F. D-18

Dodson, Helen W. D-184-187,

419

Dolbear, D.W.N. D-188

Douglas, J.N. D-189, 608,

776, 974

Dowden, R.L. D-190

Drake, Frank D. D-191, 192,

6G8

Dreese, E. E. D-409

Dueno, Braulio D-193

Easton, R.L. D-198

Edge, D. O. D-608

Efremov, A.I. D-492

Egeland, Alv D-238

Ehmert, Alfred D-199, 200, 419

Elgaroy, Oystein D-201-203,

608, 975

Elliot, H. D-151, 138, 223

Ellis, G. R.A. D-204-209

Ellison, Mervyn Archdall D-151,

210-215, 223

Elsasser, H. D-216

Elsmore, B. D-453, 608

Emberson, R. M. D-800

Engler, Nicholas A. D-823

Erickson, W.C. D-217, 608

Evans, G. O. D-308

Evans, J. V. D-165, 608

Evans, John W. D-218, 419

Evans, S. D-165, 608

Ewen, H.I. D-191

Fan, C.Y. D-219

Faust, H. D-220

Fediakina, N.I. D-977

Fedoseev, L.I. D-918

Feinstein, Joseph D-221

Fensler, W. E. D-222

Ferarro, V.C.A. D-223

Feriolo, Carl D-970

Fergusson, E. S. D-715

Fetner, E. M. D-224

Fieldhouse, P. D-151

Findlay, J. W. D-800

Firor, J. D-608

Fiskin, J. M. D-763

Fleischer, Robert D-608, 978

Fleming, John Adam D-225

Fokker, A. D. D-226-228, 608

Forbush, S. E. D-229

Forsyth, P. A. D-230

Fowler, C.S. D-101

375
Fradkin, M.I. D-426

Franklin, C.A. D-835

Fredriksen, A. D-445

Fricker, S.J. D-231

Friedman, Herbert D-125-127,

232, 668

Frihagen, J. D-233

Fuster, Arsenio D-234

Galbraith, W. D-151

Gallagher, P. B. D-976

Gallet, Roger M. D-235-238

Gardner, F. F. D-610

Garmire, G. D-514

Garriott, Owen K. D-81, 176,

239, 240, 309

Gates, David M. D-241

Gaynor, Frank D-785

Gelfreich, G.B. D-608

Gendrin, Roger D-109, 242

Gerson, Nathaniel C. D-243-

245

Getmansev, G. G. D-651

Ghose, A. K. D-246

Gibson, John E. D-247, 608

Ginzburg, V.L. D-248, 499,

608, 651, 979

Giordmaine, J. A. D-249, 608

Giovanelli, R. G. D-608

Gledhill, J. A. D-250, 251

Goh, T. D-277

Golay, M.J. E. D-252

Gold, Thomas D-151, 253,

524, 608

Goldberg, Leo D-419

Goldstein, L. D-40, 569

Goldstein, Samuel J. , Jr. D-254

Goldstone, G. T. D-190

Gonze, R. D-255

Goodman, J. D-256

Gopal Rao, M. S. V. D-257, 258

Gordon, W. E. D-259

Gorelova, M. V. D-855

Gottlieb, K. D-608

Graham Smith, F. D-260

Grant, Lewis J. , Jr. D-261

Graves, Carl D. D-262

Greenhow, J. S. D-117, 668

Greyber, H. D. D-391

Gringauz, K.I. D-263-265, 980

Groen, P. D-578

Groves, J. R.V. D-207

Gruber, S. D-266

Guier, William H. D-267

Gupta, S.K. D-246

Gustafsson, Georg D-268

Gutmann, Monique D-608

Hachenberg, Otto D-269-271

Haddock, F.T. D-272, 273,

424, 570, 575, 608

Hagen, John P. D-274-276

Hakura, Yukio D-277, 592,593

Hamburg. Meteorologisches

Observatorium D-278

Hame, T. G. D-279

Hanel, R.A. D-981

Harang, L. D-280, 281

Hargreaves, J. K. D-565

Harradan, Harry Durward

D-225

Harris, I. D-282

Harrison, V.A. W. D-283

Harrower, G. A. D-982

Hartz, T. R. D-284-286, 608

Harvard Univ. Harvard College

Observatory D-287

Harvey, Gladys A. D-147-149

Haskell, R.E. D-288

Haslam, C.G.T. D-983

Hatanaka, Takeo D-289, 290,

651

Haviland, R.P. D-291, 292

Hawkins, Gerald S. D-524

Hayre, H. S. D-293

Hazard, C. D-93, 608

Hazzaa, I. B. D-730

Hedeman, E. Ruth D-185

Heisler, L.H. D-562

Heifer, H. L. D-608

Hellgren, G. D-802

Helliwell, R.A. D-152, 237,

309, 524, 777, 778

Hepburn, Nannielou D-274

Heppner, J. P. D-104

376
Herbays, E. D-294

Herrinck, Paul D-295

Hess, H. A. D-6,

Hewish, A. D-296, 298, 608,

705

Hey, J.S. D-29, 30, 223,

299-303, 575, 608

Hibberd, F.H. D-304-306

Higgins, C.S. D-740, 745,

1007

Higgy, Robert C. D-411, 412,

415

Hill, E. R. D-995

Hill, R.A. D-197

Hilton, W.F. D-307

Hindman, J. V. D-123

Hines, CO. D-575

Hitchcock, R.J. D-308

Hogbom, J. A. D-608, 894

Hoffman, W.C. D-309

Holt, E.H. D-238

Hood, Harold C. D-310

Hope, E. R. D-54, 311

Horner, F. D-312

Houston, R.E. ,Jr.. D-313, 497

Howard, W. E. Ill D-514

Hoyle, Fred D-314, 608, 984

Huang, Chun-Ming D-315

Huang, Su-Shu D-316

Huber, P. W. D-317

Huguenin, G. R. D-189

Hughes, V.A. D-302, 608

Hulburt, E.O. D-225

Hultqvist, Bengt D-6, 318, 319

Hund, August D-320

Huntley, H. E. D-321

Hutchinson, H. P. D-322

Huxley, L.G.H. D-323

Hyde, Margaret O. D-324

Iatsunskii, I. M. D-499

Ikhsanov, R.N. D-325, 651

Ikhsanova, V. N. D-608

Ingalls, R.P. D-231, 326

Inoue, Yuji D-327

International Geophysical Year

(IGY) D-328, 329

International Scientific Radio

Union D-330

International Telecommunication

Union D-331

Israel, Hans D-332

Istomin, V. G. D-333, 985

Iwai, Akira D-334

Iwanowska, Wilhelmina D-335

Jacchia, L. G. D-336

Jackson, J. E. D-337, 725, 728

Jacobs, George D-338

James, J. C. D-326

Jansky, C. M. , Jr. D-344, 345

Jansky, Karl Guthe D-339-343

Japan. Science Council, Ionosphere Research Committee

D-346

Jasik, Henry D-347

Jastrow, R. D-282

Jaye, W. E. D-348

Jelley, J. V. D-349, 350

Jennison, R.C. D-351, 352, 608

Jesperon, James L. D-441

Jindo, Hidehiko D-812

Johler, J. R. D-143

Johnson, Francis S. D-353-355

Johnson, M.H. D-356

Johnson, W.C. D-554

Johnston, T. W. D-748

Jones, I.L. D-63, 357

Jones, Robert E. D-358, 541

Jongen, H. F. D-578

Jordan, E. C. D-570

Joy, W. R.R. D-389

Kaidanovskii, N. L. D-608

Kakinuma, Takakiyo D-359,

360, 608, 812-816

Kaidanovskii, N.L. D-608

Kallmann, H. K. D-361-363, 986

Kamiya, Yoshiko D-364

Kamiyama, Hiroshi D-365, 367

Karpov, A. N. D-366

Kato, Yoshio D-367, 368

Katzin, M. D-917

377
Kazantsev, A. N. D-369, 499

Kazes, Ilya D-27f 370-372

Kell, R.E. D-373

Kellogg, William W. D-374,

375

Kelly, Joseph J. D-376

Kelly, L.C. D-616

Kelso, John M. D-377

Keneshea, T.J. D-625

Kennaugh, E. M. D-279

Kent, G. S. D-378

Kerr, Frank J. D-379-381

Khaikin, S. E. D-382, 608,

651

Kidd, William C. D-4, 5

Kiepenheuer, Karl O. D-383

Kikuchi, Takehiko D-367

Kimpara, Atsushi D-384, 385

King, G. A.M. D-386

King, J.I.F. D-391

Kirchner, P.K. D-689

Kisliakov, A. G. D-387

Kitchen, F. A. D-389

Klee, Ernst D-390

Klein, M.M. D-391

Klinger, Hans Herbert D-392

Klinker, Ludwig D-393

Knight, Raymond M. D-480

Knuth, Robert D-393

Ko, H.C. D-394-396, 405,

407

Koeckelenbergh, A. D-397,

393

Komesaroff, M.M. D-399,

400, 987, 1007

Korol'kov, D. D-608

Korowski, E. T. D-401

Koster, J. R. D-402, 912

Kotadia, K. M. D-652

Krasovskii, V.I. D-403, 404

Kraus, John D. D-380, 405-

415

Kreplin, R. W. D-126, 127

Krishnamurthi, M. D-388, 416

Krishnan, T. D-417

Krivsky, L. D-418

Krook, Max D-523

Kruger, A. D-270

Kuiper, Gerard Peter D-419

Kunan, P.C. D-419

Kundu, Mukul Ranjan D-420-

424, 608

Kuperov, L.P. D-425

Kurnosova, L. V. D-426, 427,

767

Kurt, V.G. D-263

Kushner, Iu. M. D-404

Kuz'min, A. D. D-608, 988

Laffineur, Marius D-428-432,

848

Lambie, M. D-151

Landmark, Bjorn D-6, 433

Lange-Hesse, Giinther D-434

Larence, Robert S. D-522

Large, M.I. D-989

Lauter, Ernst August D-435-

437, 786

Lawrence, Lovell, Jr. D-438,

439

Lawrence, Robert S. D-440-

443, 471, 524

Lawson.. G.J. D-63

Leadabrand, Ray L. D-348,

444, 445

Lebedeva, P.N. D-446

Lebenbaum, M. D-256

Lee, Robert H. D-447

Lehigh Univ. Institute of Research D-448

Lehnert, Bo Peter D-449

Leighton, Hope I. D-450

Leinbach, Harold D-469, 470,

681, 990

Lejay, Pierre D-451

Lepineux, M. D-452

Lengrusser, Peter D-644

Leslie, Patricia R. R. D-453

Lied, F. D-433, 454, 455

Lilley, A. E. D-189, 456

Lincoln, J. Virginia D-457

Lindquist, Rune D-458, 459

Link, Frantsiek D-128, 608,

651

Liszka, Ludwik D-6, 472, 473,

991

378
Little, A.G. D-123

Little, C.Gordon D-240, 309,

443, 460-471, 510, 575,

773

Lodge, Sir Oliver Joseph D-474

Lovell, A.C.B. D-92, 475-479,

608, 668, 773

Low, Ward C. D-480

Lozinskaia, T.A. D-855

Ludwig, George H. D-481, 509,

840

Lugeon, Jean D-482

Lust, R. D-61

Mac Arthur, J. W. D-483

McClain, E. F. D-603

McCoy, D.O. D-484

McCready, L.L. D-610, 896,

1001

Mc Cullough, T. P. D-515, 575

Mcllwain, Carl E. D-699

Mc Intosh, Douglas Haig

D-485

McKerrow, C.A. D-486

Mc Lean, D. J. D-487, 992

Mc Math, R. R. D-419

Mc Narry, L. R. D-149

Mc Vittie, G. C. D-608

Magnuson, G. D. D-488

Makhailov, A. A. D-499

Malik, Chester D-489

Malinge, Anne-Marie D-490

Malurkar, S.L. D-491

Mambo, Masayoshi D-838

Mandel'shtam, S.L. D-492

Manning, Lawrence A. D-570

Marini, J. W. D-493 * Marmo, F. F. D-494

Marner, Gene R. D-495, 496

Marsden, P.L. D-151

Marshall, Alan C. D-497

Martin, L.H. D-ll

Martyn, D. F. D-493

Mason, W.C. D-231

Massachusetts Institute of Technology. Lincoln Laboratory

D-499

Massey, H. S. W. D-500-505

Mather, Robert A. D-994

Mathewson, D. S. D-124, 608,

989

Matsushita, Sadami D-506-508

Matthews, Whitney D-509

Maxwell, Alan D-461, 463,

510-514, 524, 830

Mayer, Cornell H. D-248, 515,

575, 608

Mayer, H. F. D-516

Mechtly, E. A. D-517

Medd, W.J. D-518

Medved, D.B. D-488, 519

Meinel, A. B. D-520

Meltz, G. D-700

Menzel, Donald Howard D-521-

524

Menzel, Willi D-558

Merrill, Harrison J. D-525

Merritt, Robert P. D-468

Merson, R.H. D-526

Metzger, P. G. D-527

Michigan Univ. Engineering Research Institute D-528

Mickelwait, Aubrey B. D-529

Mikhnevich, V. V. D-499

Milerova', A. D-756

Miller, Raymond J. D-993

Millman, George H. D-530,

531, 994

Mills, B.Y. D-608, 611, 995

Mimno, Harry Rowe D-532

Miner, Richard Y. D-533

Minkowski, R. D-608

Minnaert, M.G.J. D-419, 578,

608

Minnett, H.C. D-628, 629

Minnis, CM. D-534-540

Mitchell, F.H. D-892, 893

Mitra, A. P. D-541-545, 741,

996

Mitra, S. K. D-546, 547

Mitra, S.N. D-548, 729

Miyazaki, Yukio D-549

Moller, F. D-550

Molchanov, A. P. D-608, 997

Molozzi, A. R. D-110, 835, 971

379
Moody, Alton B. D-551

Mook, Conrad P. D-552

Moorcroft, D. R. D-553

Moore, Charlotte E. D-419

Morgan, M.G. D-13, 554

Moroz, V.I. D-263

Morrison, Philip D-136

Muldrew, D. B. D-369

Mullaly, R.F. D-417

Milliard Radio Astronomy Observatory, Cambridge,

England D-555

Muller, C.A. D-556, 608

Muller, Hans-Gerhard D-557

Muller, Rolf D-558

Munro, G.H. D-559-562

Murcray, W. B. D-563, 564

Murray, W. A. S. D-565

Nagoya, Japan. Univ. Research

Institute of Atmospherics

D-566, 567

Naismith, R. D-308, 568, 998

Narasinga Rao, K. V. D-569

Narayana, J. V. D-163

Narayana Rao, N. D-783

Narlikar, J. V. D-984

National Research Council, Wash.,

D. C. United States National

Committee of the International

Scientific Radio Union

(ISRU) D-570-575

Nazarova, T.N. D-499

Neishild, V.G. D-446

Nelson, J. H. D-576

Nesmeianov, A. N. D-577

Netherlands. Meteorologisch

Instituut D-578

Netherlands. Telecommunications

Services, The Hague D-579

Newell, Homer E. , Jr. D-580, 581,

663

Newkirk, G. , Jr. D-608

Newton, H. W. D-223, 582, 583

Nichols, J.H. D-575

Nicolet, Marcel D-584-586, 668

Nisbet, John S. D-587

Nordberg, W. D-799

Nordo, Jack D-588

Noton, A. R. Maxwell D-999

Obayashi, Tatsuzo D-589-

593

Okhotsimskii, D. E. D-499

Oort, J.H. D-578, 603

Ordway, F.I. D-594

Orhaug, T. D-433

Ortner, Johannes D-319

Osborne, C.B. D-595

Outsu, Jinsuke D-334

Ovenden, Michael W. D-596

Owren, Leif D-185, 575, 599

Paetzhold, H. K. D-598-605

Palmer, C.E. D-606

Palmer, D. R. D-151

Palmer, H.P. D-163, 575

Panovkin, B.N. D-446, 608

Papaleksi, H. D. D-607

Pariiskii, Iu. N. D-1000

Paris Symposium on Radio

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1958 D-608

Park, Robert A. D-529

Patterson, T. N.L. D-609

Paulson, K. V. D-230

Pawsey, J.L. D-419, 608,

610-613, 1002

Payne-Scott, Ruby D-1001

Pecker, Jean-Claude D-614

Pedersen, K. D-280

Penico, A.J. D-615

Pepper, J. D-212

Perers, O. D-802

Perkins, W. H. D-770

Perlman, S. D-616

Peterson, Allen M. D-524, 617

Peterson, L.E. D-618

Petri, Winfried D-94, 619-

621

Pettengill, Gordon H. D-622

Pfeiffer, John D-623

380
Pfister, Wolfgang D-309,

624-826

Pick-Gutmann, Monique

D-38, 39, 627

Piddington, J. H. D-628-630

Piggott, W. R. D-31, 582,

631, 632

Picker ner, S.B. D-651

Pineo, V.C. D-1003

Pisareva, V. V. D-633

Poeverlein, Hermann D-489,

634

Poincelot, Paul D-635

Poloskov, S.M. D-499

Ponomarev, E. A. D-1004

Pope, Joseph H. D-563, 564,

636-638

Porter, N. A. D-151

Porter, Richard W. D-639

Pourbaix, E. D-255

Powell, C.F. D-640

Pravda, Moscow D-641

Pressey, B. G. D-559

Pressman, J. D-494

Preston, George W. D-78

Prew, Henry E. D-642

Price, R. D-787

Priester, W. D-643-646

Primich, R.I. D-647

Rabben, H. H. D-648

Radhakrishnan, V. D-649, 650

Radio Astronomy Symposium,

Jodrell Bank, Aug. 1955

D-651

Rajan, V. D. D-46

Ramachandra Rao Pant, P.

D-258

Ramanathan, K. R. D-59, 60,

652-654

Rand, S. D-655, 656

Rao, B. Ramachandra D-257,

258, 657-659

Rastogi, R. G. D-652, 660-662

Ratcliffe, J. A. D-97, 663-868,

707, 1005

Rawer, Karl D-6, 669-672

Ray, S. D-711

Rayton, W. M. D-465, 466

Razorenov, L. A. D-426

Reber, Grote D-673-680

Reid, George C. D-681-684,

990

Reid, J.H. D-151

Revellio, K. D-199, 200

Reyssat, M. D-109

Richey, Frances D-685

Ringnes, Truls S. D-686

Rishkov, N. D-608

Rix, H.D. D-687

Robbins, A. R. D-829

Roberts, C. A. D-688

Roberts, C. R. D-689

Roberts, J. A. D-608, 649,690-

692, 900, 901

Roberts, Walter Orr D-419, 893

Rochelle, R. W. D-694

Rodgers, M.F. D-959

Rodman, Richard B. D-751

Roelofs, R. D-578

Roger, R.S. D-6

Roman, Nancy G. D-608, 913

Roof, R.B. D-465, 466

Rosen, A. D-695

Ross, W.J. D-313, 696, 697

Rosseland, Svein D-698

Rothwell, Pamela D-699

Rotman, W. D-700

Rougoor, G. W. D-608

Roy, K. M. D-246

Rudakov, V. A. D-264

Rudkjobing, Mogens D-701

Rumi, G. C. D-468

Russel, W.J. D-616

Rutherford, G. T. D-1006

Ryan, W. D. D-702

Rybner, Jorgen D-703

Rydbeck, Olof E. D-704

Ryle, Martin D-608, 705-709

Sadler, D.H. D-710

Sagalyn, Rita C. D-309

Saha, A.K. D-711

Sanamian, V. A. D-608

381
Sanders, Armand E. D-994

Sarada, K. A. D-712, 996

Scanlon, T. F. D-608

Schaetti, N. D-44

Schatzman, E. D-608

Scheer, Donald J. D-411

Scheffler, H. D-713

Schiffmacher, E. R. D-714

Schilling, G.F. D-715

Schindelhauer, F. D-716

Schmelovsky, Karl Heinz

D-393, 717

Schmerling, E. R. D-313, 575

Schmidt, H. D-718

Schwentek, Heinrich D-719

Scott, James C. W. D-720

Seddon, J.Carl D-309, 575,

721-728

Sedra, R.N. D-730

Seeger, Charles L. D-731, 732

Sen, Hari K. D-733

Sen, S.N. D-734

Sen Gupta, Prabhat K. D-729

Sengupta, Dipak L. D-735

Senior, T.B.A. D-222, 608,

736, 737

Senn, George D-755

Seshagiri, Rao T. D-388, 416

Sethumadhavan, K. D-162

Setty, C.S. G. K. D-738

Shain, C.A. D-379, 380, 400,

608, 651, 739-745, 1007

Shakeshaft, J. R. D-608

Shapiro, B. S. D-17

Shapiro, I. R. D-104

Sharma, S. K. D-45

Shearman, E. D. R. D-42

Shepherd, W. G. D-570

Sheridan, K. V. D-608, 904,

905

Shibata, Hisashi D-748, 838

Shkarofsky, I. P. D-747, 748

Shklovskii, I.S. D-651, 749-753

Shternfel'd, A. A. D-754

Shuter, W.L.H. D-972

Siedentopf, H. D-53

Siegel, K. M. D-222, 608, 738,

737

Siglin, Pierce W. D-755

Simaljak, J. D-756

Simon, Paul D-37, 608, 757

Simpson, J. A. D-419

Singer, S.Fred D-758-761

Sinton, William M. D-762

Sisco, W.B. D-763

Sivarama Sastry, G. D-388, 416

Sivaramakrishnan, M. V. D-764

Six, F. D-772

Skeib, G. D-436, 765

Skilling, William Thompson

D-766

Skinner, N.J. D-912

Skribeland, S. D-433

Skuridin, G. A. D-767

Slee, O.B. D-768, 995

Sloanaker, R. M. D-515, 575,

608

Slonim, Iu. M. D-769

Smerd, S. F. D-419

Smith, Alex G. D-770-772

Smith, Ernest K. , Jr. D-575

Smith, F. Graham D-575, 608,

611, 773-775

Smith, Harlan J. D-608, 776,

974

Smith, P. A. D-998

Smith, R.L. D-777, 778

Smith-Rose, R.L. D-779

Smyth, John B. D-570

Soboleva, N. S. D-608

Sorensen, E. V. D-780

Soifer, Raphael D-781

Solar eclipses and the ionosphere

(Sympos ium ) D-782

Somayajulu, Y. V. D-783

Sonett, C.P. D-695

Southworth, George C. D-784

Spitz, Armand D-785

Sprenger, K. D-436, 786

Stableford, C.V. D-80

Stankevich, K. S. D-651

Stanley, G.J. D-691, 787, 966

Staras, H. D-788

Steinberg, Jean-Louis D-27, 65,

66, 370-372, 608

Steinhauser, F. D-212

Sternberg, Sidney D-789

Stetson, Harlan T. D-790

382

aaaaa
Stiltner, Ernest D-468, 683

Stodola, E. K. D-180

Stoffregen, W. D-791

Stolarik, J. D. D-104

Stone, M.L. D-326

Storey, L.R.O. D-575, 792-

794

Storey, Owen D-795

Stoutenburgh, D.V. D-407

Straka, Ronald M. D-4

Stranz, Dietrich D-796

Strassl, H. D-527

Stratton, F. J. M. D-797

Strick, H. D-895

Stromgren, Bengt D-419

Strong, C.L. D-798

Stroud, W. G. D-799, 981

Struve, O. D-800

Stuart, W.D. D-616

Stumpers, F. L. H. M. D-732

Surange, P. G. D-45

Suzuki, Shigemasa D-801

Svensson, S.I. D-802

Svetlitskii, E. M. D-404

Swamp, G. D-513, 524, 803

Swenson, G. W. , Jr. D-915

Swerling, Peter D-804, 805

Swift, D. W. D-1008

Symposium on Ballistic Missiles and Space Technology,

4th, 1959 D-806

Symposium on Physical Processes in the Sun-Earth

Environment D-807

Symposium on the Plasma

Sheath: Its effects on communication and detection,

Dec. 1959 D-808

Syrovatskii, S.I. D-809

Takakura, Tatsuo D-608

Takayanagi, Toshio D-812

Takeuchi, Hajime D-549

Tanaka, Haruo D-608, 812-816

Tandberg-Hanssen, Einar

D-698, 817, 818

Tandon, Jagdish Narain D-819

Taratynova, G. P. D-499

Tatel, H.E. D-608

Taubenheim, Jens D-820, 821

Taylor, Eloise W. D-822

Taylor, Paul B. D-823

Taylor, William C. D-824, 825

Technical Document Liason

Office, Wright Patterson

Air Force Base, Ohio

D-754

Theissing, H. H. D-826, 827

Thomas, J. A. D-306, 828

Thomas, J. O. D-575, 829

Thompson, A. R. D-513, 524,

608, 830

Thomson, J. D-6

Thomson, J. H. D-608

Tischer, F.J. D-831

Tompkins, Edwin H. , Jr. D-529

Tousey, R. D-419

Tovmasian, H. M. D-608

Townes, C.H. D-248, 608

Trent, G. H. D-608

Trexler, James H. D-832

Triska, P. D-437

Triskova, Ludmila D-833

Troim, J. D-6, 233, 281

Troitskii, V. S. D-651, 918

Tunmer, Harriet D-608

Twiss, R.Q. D-834

Tyas, J.P.I. D-835

Udal'tsov, V.A. D-608

Ulwick, J.C. D-626

Ungstrup, Emil D-703

U. S. Dept. of the Army, Army

Library D-836

U. S. Weather Bureau D-1009

Utah. University D-837

Utlaut, W.F. D-238

Uyeda, Hiroyuki D-838

383
Vakhnin, V. D-499

Van Allen, James A. D-839,

840

van Bladel, J. D-841

van de Hulst, H. C. D-4, 608

van Hurck, N. D-732

Van Isacker, J. D-842

Van Sabben, D. D-843, 850

Van Woerden, H. D-608

Varsavsky, Carlos M. D-751

Vassy, Etienne D-6, 844-847

Vauquois, Bernard D-608, 848

Vavilov, V.S. D-499

Veldkamp, J. D-578, 849, 850

Vening Meinesz, F. A. D-578

Venugopal, V. R. D-851

Verdeyen, J. T. D-569

Vernov, S.N. D-499

Vestine, E.H. D-668, 1010

Vilbig, Friedrich D-852

Villard, O.G. , Jr. D-153, 176

Viterbi, A.J. D-853

Vitkevich, V.V. D-608, 651,

854, 855

Vogelman, Joseph H. D-856"

Voigt, H.H. D-857-861

Volders, Louise D-608

Volland, Hans D-271, 862

von Eshleman, R. D-524, 976

Von Kliiber, H. D-863

Votaw, M.J. D-198

Wachtler, Maximilian D-864

Wait, James R. D-865, 866

Waldmeier, Max D-608, 867,

868

Wallis, G. D-608

Walsh, D. D-608

Wang, Shou-Kuang D-608

Warren, E. D-869

Warwick, Constance D-608,

870, 871

Warwick, James W. D-67, 522,

608, 872-877, 1011

Watanabe, Tomiya D-368

Watkins, CD. D-575, 1012

Watts, J. M. D-878, 879

Weber, Ernst D'-570

Webster, H.C. D-880

Weekes, K. D-9, 151, 223,

668

Wehner, R. S. D-685

Weiffenbach, George C. D-267

Weisbrod, S. D-881

Wells, H. W. D-118, 882, 883

Westerhout, Gart D-575, 608,

884, 885

Westfall, W.D. D-886

Wexler, Raymond D-887

Whale, H.A. D-888

Wheelon, A. D. D-889

Whelpley, William A. D-481

Whipple, FredL. D-890

White, R.B. D-561

Whitehead, J. D. D-430, 891

Whitehurst, R.N. D-892, 893

Whitfield, G. R. D-608, 894

Whitney, H.E. D-6, 895

Wild, J.G. D-419

Wild, J. P. D-608, 896-905,992

Wild, P.A.T. D-972

Williams, W.E. , Jr. D-906

Wilson, D. McL.A. D-908

Wilson, J.G. D-151

Wilson, Raymond H. , Jr. D-907

Winckler, J. R. D-618

Witunski, Michael D-909

Wolff, E.A. D-917

Wong, Ming S. D-910

Wood, Marion D-175, 871

Woodward, R.H. D-911

Wright, R.W. D-912

Wrigley, F. D-575

Yabroff, I. W. D-778

Yaplee, B. S. D-575, 608, 913

Yates, G.C. D-98

Yee, James S. D-914

Yeh, K.C. D-915

Yeh, L.P. D-916

384
Zachary, W. W. D-917

Zakharov, G. F. D-404

Zelinskaia, M. R. D-918

Zevakina, R.A. D-919

Zirin, Harold D-874, 875

Zhekulin, L. A. D-920

Zhelezniakov, V. V. D-921

Ziegler, H. K. D-922

Zschomer, H. D-598, 602

Anonymous D-923-958, 1013

tt U.S. GOVERNMENT PRINTING OFFICE: 1963 O - 680381

385

U. S. DEPARTMENT OF COMMERCE

Luther H. Hodges, Secretary

NATIONAL BUREAU OF STANDARDS

A. V. Astin, Director THE NATIONAL BUREAU OF STANDARDS

The scope of activities of the National Bureau of Standards at its major laboratories in Washington, D.C., and

Boulder, Colorado, is suggested in the iolk-.wing listing of the divisions and sections engaged in technical work.

In general, each section carries out specialized research, development, and engineering; in the field indicated by

its title. A brief description of the activities, and of the resultant publications, appears on the inside of the

front cover. WASHINGTON, D.C.

Electricity. Resistance and Reactance. Electrochemistry. Electrical Instruments. Magnetic Measurements

Dielectrics. High Voltage.

Metrology. Photometrj and Colorimetry. Refractometry. Photographic Research. Length. Engineering Metrology.

Mass and Scale. Voiumetry and Densimetry.

Heat. Temperature Physics. Heat Measurements. Cryogenic Physics, Equation cf State. Statistical Physics.

Radiation Physics. X-ray. Radioactivity. Radiation Theory. High Energy Radiation. Radiological Equipment.

Nucleonic Instrumentation. Neutron Physics.

Analytical and Inorganic Chemistry. Pure Substances. Spectrochemistry. Solution Chemistry. Standard Refer- ence Materials. Applied Analytical Research, Crystal Chemistry.

Mechanics. Sound. Pressure and Vacuum. Fluid Mechanics. Engineering Mechanics. Rheology. Combustion

Controls. Polymers. Macromolecules: Synthesis and Structure. Polymer Chemistry. Polymer Physics. Polymer Characterization. Polymer Evaluation and Testing. Applied Polymer Standards and Research. Dental Research.

Met&SJurgy. Engineering Metallurgy. Microscopy and Diffraction, Metal Reactions. Metal Physics, Electrolysis and Metal Deposition.

Inorganic Solids. Engineering Ceramics. Glass. Solid State Chemistry. Crystal Growth. Physical Properties.

Crystallography.

Building Research. Structural Engineering. Fire Research. Mechanical Systems. Organic Building Materials. Codes and Safety Standards. Heat Transfer. Inorganic Building Materials. Metallic Building Materials. Applied Mathematics. Numerical Analysis. Computation. Statistical Engineering. Mathematical Physics. Operations Research. Data Processing Systems. Components and Techniques. Computer Technology. Measurements Automation; Engineering Applications. Systems Analysis.

Atomic Physics. Spectroscopy. Infrared Spectroscopy. Far Ultraviolet Physics. Solid State Physics. Electron Physics. Atomic Physics. Plasma Spectroscopy.

Instrumentation. Engineering Electronics. Electron Devices. Electronic Instrumentation. Mechanical Instru- ments, Basic Instrumentation. Physical Chemistry. Thermochemistry. Surface Chemistry. Orgastic Chemistry. Molecular Spectroscopy. Ele- mentary Processes. Mass Spectrometry. Photochemistry and Radiation Chemistry.

Office of Weights and Measures. BOULDER, COLO.

Cryogenic Engineering Laboratory. Cryogenic Equipment. Cryogenic Processes. Properties of Materials. Cryogenic Technical Services. CENTRAL RADIO PROPAGATION LABORATORY

Ionosphere Research and Propagation. Low Frequency and Very Low Frequency Research. Ionosphere Research. Prediction Services. Sun-Earth Relationships. Field Engineering. Kadio Warning Services. Vertical Soundings Research.

Radio Propagation Engineering. Data Reduction Instrumentation. Radio Noise. Tropospheric Measurements.

Tropospheric Analysis. Propagation-Terrain Effects. Radio-Meteorology. Lower Atmosphere Physics.

Radio Systems. Applied Electromagnetic Theory. High Frequency and Very High Frequency Research. Fre- quency Utilization. Modulation Research. Antenna Research. Radiodetermination.

Upper Atmosphere and Space Physics. Upper Atmosphere and Plasma Physics. High Latitude Ionosphere

Physics. Ionosphere and Exosphere Scatter. Airglow and Aurora. Ionospheric Radio Astronomy.

RADIO STANDARDS LABORATORY

Radio Physics. Radio Broadcast Service. Radio and Microwave Materials. Atomic Frequency and Time-Interval

Standards. Radio Plasma. Millimeter-Wave Research.

Circuit Standards. High Frequency Electrical Standards. High Frequency Calibration Services. High Frequency

Impedance Standards. Microwave Calibration Services. Microwave Circuit Standards. Low Frequency Calibration

Services.