bluuebunny/crossref_metadata_2025 huggingface dataset:
Tucson Magnetic Observatory January to March, 1946
Authors: Westerman C. Edward
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)

January 3–4—A magnetic storm of moderate intensity began at 07h 00m GMT, January 3. During the first eight hours of the storm the activity was mainly a long‐period variation of D and H. From 15h to 17h, January 3, there were very rapid variations. For the next eighteen hours activity was slight, but with a markedly depressed H. The storm ended about the middle of the Greenwich day, January 4. Ranges: D, 21′.5; H, 197 gammas.
Huancayo Magnetic Observatory January to March, 1946
Authors: Ledig Paul G.
Published: February 2008

(Latitude 12° 02′.7 S., longitude 76° 20′.4 or 5h 01m.4 W. of Gr.)

January 3—A short but very strong magnetic storm began at 08h 07m GMT, January 3, with a 50‐gamma increase of H in six minutes, followed by almost four hours of very moderate, small movements. Then at 12h 05m a deep bay began with its minimum at 12h 40m, followed by over an hour's slow increase and then a sharp, narrow peak at 14h 25m and another peak at 15h 38m, which was the maximum of the day—367 gammas above the base‐line. There was a narrow, deep bay at 16h 35m and a series of small, deep bays on a low in H which lasted from about 18h to 21h. The minimum of the day was at 19h 43m—96 gammas below the base‐line—and the range for the day was 463 gammas. As usual, H‐values for several days were below normal, and D and Z were only mildly disturbed with small, sharp movements.
The Royal Magnetic and Meteorological Observatory, Batavia
Authors: Berlage H. P.
Published: February 2008

From April 1, 1946, the Royal Magnetic and Meteorological Observatory was transferred from the Navy Department to the Department of Public Works and Communications, Batavia‐C. I beg all correspondents to use the new address immediately after reception of this circular letter.

During the Japanese occupation the most valuable part of the Observatory Library was removed by the Japanese. Moreover acquisitions stopped for more than four years. To every institute which is in the position to cooperate and help to recover this library I urgently request that copies be forwarded of all its publications in the domain of meteorology and geophysics.
Apia Observatory, western Samoa January to June, 1946
Authors: Beagley J. W.
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)

January 3–4—A sudden commencement at 08h 09m GMT, January 3, marked the beginning of a moderate disturbance. This was followed by irregular fluctuations gradually diminishing until 09h 45m, January 4. On January 3, K‐indices of 5, 5, and 6 were recorded during the third, fourth, and sixth intervals and on January 4 K‐indices of 5 occurred during the third and fourth intervals.
Watheroo Magnetic Observatory April to June, 1946
Authors: Wood F. W.
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)

April 22–24—A moderate disturbance began with a sudden commencement at 07h 00m GMT, April .22, with an increase in H of 37 gammas in four minutes, although the storm was well shown in all of the elements. The traces were only slightly disturbed during the ensuing twenty‐two hours, the horizontal intensity beginning to decrease at 05h, April 23. Unfortunately, at 06h 20m the recording lamp burned out and was replaced at 09h, by which time the horizontal intensity had decreased by 73 gammas and large, sweeping movements were in progress. These movements continued until 18h, April 24, the times of greatest activity being between 16h to 18h, April 23, 00h to 06h and 10h to 12h, April 24. The traces were normal by midnight, April 24. A faint aurora was seen in Perth in the evening of April 24. Ranges: D, 29′; H, 285 gammas; Z, 196 gammas.
Solar and magnetic data, April to June, 1946, Mount Wilson Observatory
Authors: Nicholson Seth B. , Sternberg Mulders Elizabeth E.
Published: February 2008

The magnetic storm of April 22–24 began when an active bipolar sunspot‐group, Mount Wilson No. 8026, was 50° east of the central meridian, in latitude 33° north. Two solar flares were observed in this group on April 22, one 8 hours, the other 13 hours after the storm began.

When the magnetic storm of May 5–7 began, groups 8033, 8038, and 8039 were west of the central meridian, having crossed it on May 4.3, 4.5, and 5.3, respectively. Solar flares were observed in No. 8038 on May 2, 3, and 7.
American magnetic character‐figure, CA, three‐hour‐range indices, K, and mean K‐indices, KA, for July to September, 1946
Authors: Scott W. E.
Published: February 2008

Summaries of American URSI broadcasts have appeared regularly in this Journal since the issue for December, 1930.

As set forth in this Journal for June, 1937, “The Department of Terrestrial Magnetism and the United States Coast and Geodetic Survey with the cooperation of the United States Army and the United States Navy communication‐services and several amateur radio stations have undertaken to supply the American character‐figure based upon the reports of the seven American‐operated observatories—those of the Department of Terrestrial Magnetism at Huancayo in Peru and at Watheroo in Western Australia, and those of the United States Coast and Geodetic Survey at Cheltenham (Maryland), Honolulu (Hawaii), San Juan (Puerto Rico), Sitka (Alaska), and Tucson (Arizona).” This character‐figure is being designated CA, and its values for the first twelve, the second twelve, and all twenty‐four hours of each Greenwich day for July to September 1946, are given in Table 1.
Summary report on the Extraordinary General Assembly of the International Union of Geodesy and Geophysics (IUGG), Cambridge, England, July 29 to August 2, 1946
Authors: Stagg J. M.
Published: February 2008

The following summary of the proceedings of the Extraordinary Assembly at Cambridge is abstracted from the Report prepared by General Secretary Stagg. The Report will be published in full by the Union, but meanwhile it seems desirable to acquaint readers of the Journal with the proceedings and actions taken.

Delegates—The following countries were represented by delegates: Belgium; Canada; Denmark; France; Great Britain; Holland; India; Indo‐China; Italy; Jugoslavia; Morocco; Norway; Peru; Sweden; Switzerland; and the United States of America. Apologies for absence were received from Finland, Greece, South Africa, and Turkey.
Committee on Coordination of Cosmic‐Ray Investigations
Authors: Fleming J. A.
Published: February 2008

This Committee, whose members have been W. S. Adams, J. A. Fleming, and F. E. Wright since formation by the President of the Carnegie Institution of Washington in December, 1932, to coordinate research on cosmic rays supported by the Institution, has submitted its fourteenth and final annual report for the year ended June 30, 1946. With the retirement from active service in the Institution on or before June 30, 1946, of its three members, the Committee recommended to President Bush that, effective July 1, 1946, (1) administration of its then uncompleted activities be made the responsibility of the Department of Terrestrial Magnetism of the Institution, and (2) funds still available from past appropriations be set aside, in accordance with the approved projects listed below, for disbursement by that Department through its Director. The President approved these recommendations and future reports on the completion of projects sponsored by the Committee will be made in the annual reports of the Director of the Department of Terrestrial Magnetism.

As has been indicated in the annual reports of the Committee from 1940, relatively large progress could not be made during the war years. In view of the fundamental importance of this branch of physics, this limited progress, as one would expect, has raised more questions than answers. With the cessation of hostilities and the eventual reconversion from wartime to peacetime efforts of the investigators in the field of cosmic radiation, it may well be expected that research will be vigorously resumed, particularly in the investigation of high‐energy radiations to which natural cosmic radiation gives an immediate avenue of approach. Thereby we may expect to learn basic facts by which to check theories of nuclear forces and interactions between radiation and matter.
Solar and magnetic data, July to September, 1946, Mount Wilson Observatory
Authors: Nicholson Seth B. , Mulders Elizabeth Sternberg
Published: February 2008

An immense complex bipolar sunspot‐group, Mount Wilson No. 8129, crossed the solar disk from July 19 to August 2. Its maximum area, measured at the United States Naval Observatory, was 3685 millionths of a solar hemisphere (4325 million square miles). A small flare was observed at Mount Wilson over the group on July 21 at 15h 11m GCT and a very intense one on July 25 from 16h 21m to 18h 30m.

On July 26, a great magnetic storm began at 18h 47m (from Tucson magnetogram), more than 26 hours after the appearance of the bright flare of July 25 which showed on a spectroheliogram at 16h 21m but not on one at 16h 05m. An aurora, observed at Mount Wilson near midnight of July 26 (July 27d08h), and the small magnetic storm on July 29–30 also were probably associated with this immense group.
Echoes at D‐heights with special reference to the Pacific Islands
Authors: Ellyett C. D.
Published: February 2008

Radio echoes obtained from an equivalent height of 50 km above Pitcairn Island by the usual vertical incidence pulse technique are attributed to D‐layer reflections. Previous literature has been collected, and many conflicting statements on the occurrence and behaviour of D‐layer echoes are revealed.

A total of 1302 observations of the layer, taken at Pitcairn Island between October 1, 1944, and November 16, 1945, have been analysed, showing:

(i) A frequency‐range largely contained between 2.5 and 5.0 Mc;

(ii) Occurrence during 65 per cent of all daytime observations, although night occurrence is not excluded;

(iii) Both a summer and a winter minimum of activity;

(iv) A strength of approximately one‐third the E‐layer‐echo strength, and all the typical characteristics of a sporadic region.

Similar echoes have been reported from Raoul Island (Kermadec Group) during approximately 75 per cent of the daytime in the summer of 1944–45, and from Christmas Island during 87 per cent of the daytime in the period June 11–30, 1945. It is considered that the echoes may be characteristic of a tropical region.
Daily International magnetic character‐figures, C, for the years 1884 to 1889
Authors: Bartels J.
Published: February 2008

The long series of International magnetic character‐figures C extends from 1884. The figures for 1884–89, as far as is known have never been published. The values for the six years are submitted therefore for publication in the Journal.
The vehicular odograph
Authors: McNish A. G. , Tuckerman Bryant
Published: February 2008

A description is given of the vehicular odograph, a device for automatically plotting the course of a vehicle in which the odograph is mounted. The odograph derives information on direction from a magnetic compass which is read by a photoelectric system and information on distance from a shaft geared to the speedometer‐cable. Errors in maps obtained with the device amount to two or three per cent of the total distance traveled under ordinary rough conditions of operation, but with the exercise of certain precautions these errors can be greatly reduced. Detailed discussion on the operation and compensation of a magnetic compass in a vehicle, with particular emphasis on problems of sub‐permanent magnetization is included, together with a theoretical analysis of the integrating process employed which involves averaging of discrete intervals.
Ionospheric studies in South Africa Telecommunications Research Laboratory ionospheric sounder
Authors: Wadley T. L.
Published: February 2008

The South African Council for Scientific and Industrial Research (CSIR) has recently embarked on a program for recording ionospheric heights and critical frequencies in South Africa, and, in collaboration with other ionospheric bureaus, provides a forecasting service for local users.

Two recording stations have been installed—one in Johannesburg and the other near Cape Town. Data from these two stations are analysed by the staff of the Telecommunications Research Laboratory (TRL) of the CSIR, and, in addition to being used as a basis for local forecasting, are circulated to the United Kingdom, Canada, United States of America, Australia, New Zealand, and India. Reciprocal information from these centres is also received.
Tucson Magnetic Observatory October to December, 1946
Authors: Westerman C. Edward
Published: February 2008

(Latitude 32° 14′.8 N., longitude 110° 50′.1 or 7h 23m.3 W. of Gr.)

October 26–27—A moderate storm began without sudden commencement during the first half of the Greenwich day, October 26. The greatest activity occurred between 22h on the 26th and 12h on the 27th, and the storm continued until the end of October 27, Greenwich time. Ranges: D, 14′.5; H, 155 gammas; Z, 42 gammas.
Zô‐Sè Observatory September to December, 1946
Authors: Burgaud M.
Published: February 2008

(Latitude 31° 06′ N., longitude 121° 11′ or 8h 04m.45 W. of Gr.)

September 16–24—The equinoctial magnetic activity began at 13h 47m GMT, September 16, with an abrupt rise of 15 gammas in H which was followed by a moderate disturbance with an amplitude of 120 gammas lasting some eighteen hours. At 23h 51m, September 17, sudden commencement of a major storm occurred. H swiftly decreased by 210 gammas in two hours and moderate oscillations followed around that low value during four hours, then was a new decrease of 100 gammas. Disturbed conditions prevailed with irregular oscillations and increasing values in the morning of September 18. At 12h 10m there was a new fall of the curve by 135 gammas; milder conditions continued until 14h 56m on the 18th, when a rapid increase of 140 gammas in forty minutes and two large oscillations exceeding 100 gammas brought the curve near normal values. At 10h 10m, September 19, an increase in the activity was noted and two large oscillations of 80 gammas in range. Smooth conditions prevailed thereafter. The evening of September 20 and the morning of the 21st were calm. At 17h 13m, September 21, a new, very sharp beginning of 49 gammas preceded the major storm of the equinox. Activity at first was reduced till 04h 23m September 22, when a new rise of 20 gammas was followed by a drop of 170 gammas and the curve was slowly recovering when a violent sudden start of 45 gammas took place at 10h 11m with rapid and spasmodic fluctuations during more then eight hours. The storm was then at its maximum. Disturbance abated in the evening of the 23rd and calm was absolute near 17h of the 24th.
Apia Observatory July to September, 1946
Authors: Beagley J. W.
Published: February 2008

(Latitude 13° 48′.4 S., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)

July 7–9—Minor activity commenced at 03h 27m GMT, July 7, and continued until 10h 07m, July 9. K‐indices of 5 and 4 were recorded.
Watheroo Magnetic Observatory October to December, 1946
Authors: Wood F. W.
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)

October 20—A moderate disturbance began at 03h 09m GMT, October 20, with a fairly sudden commencement. The horizontal intensity dropped by 7 gammas, then increased by 23 gammas within two minutes. D increased by 2′, then decreased to normal, while Z rose 10 gammas and then slowly decreased. The disturbance in all elements was not very great and consisted of somewhat rapid fluctuations superimposed upon larger and slower movements. Quiet conditions prevailed again by 23h. Ranges: D, 14′; H, 69 gammas; Z, 77 gammas.
Five International quiet and disturbed days for July to December, 1946
Authors: Scott W. E.
Published: February 2008

Reports of geomagnetic activity for the last six months of 1946 have been received from a sufficient number of magnetic observatories so that the international quiet and disturbed days can be selected in accordance with the method outlined on pages 219–227 in the December, 1943, issue of this Journal. The selection is based on the reports of magnetic character on a scale of 0, 1, and 2 from an average of 34 observatories and of K‐indices from an average of 27 observatories.
Solar and magnetic data, January to March, 1947, Mount Wilson Observatory
Authors: Nicholson Seth B.
Published: February 2008

An immense complex bipolar sunspot group. Mount Wilson No. 8438, crossed the solar disk from March 3 to 16. It was the second largest spot group ever recorded, having been surpassed in size only by the great group of February 1946. Group 8438 was a return or at least an outgrowth of a large group, No. 8392, which crossed the solar disk from February 5 to 18.
Witteveen Magnetic Observatory January to March, 1947
Authors: van Lohuixen H. P. Th.
Published: February 2008

(Latitude 52° 48′.8 N., longitude 6° 40′.1 or 0h 26m.7 E. of Gr.)

January 2—A minor disturbance occurred between 15h and 21h GMT, resulting in one K‐index of 5.
Cheltenham Magnetic Observatory January to March, 1947
Authors: Wiles William E.
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)

January 25–26—Following a day of slight disturbance, a storm of moderate intensity began at about 03h GMT, January 25, the major part of the disturbance occurring between 03h and 16h, January 25, and consisting of long‐period, irregular oscillations of moderate amplitude in all three elements. The perturbations continued on a diminished scale subsiding at about 15h, January 26. Minimum H was 18,072 gammas at 15h 11m, January 25. On January 25 the K‐sum was 36, three fives and one six being scaled.
Zô‐Sè Observatory January to March, 1947
Authors: Burgaud M.
Published: February 2008

(Latitude 31° 05′.8 N., longitude 121° 11′.2 or 8h 04m 45s E. of Gr.)

January 1–2—At 03h 12m and 09h 00m GMT, January 1, there were two small abrupt changes followed by small disturbances during January 1 and 2.
Differential‐penetration theory
Authors: Eckersley T. L.
Published: February 2008

There is a good deal of evidence for the existence of differential penetration. It explains a number of things which are otherwise difficult to account for.

An attempt is made, in this paper, to develop this basic idea of differential penetration. It is this:

We assume a neutral cloud of electrons and positive particles, of dimensions large compared with the Earth, coming in to the Earth, probably from the Sun, possibly from neutral clouds in space.
K‐indices, April to June, 1947, and sudden commencements, January to June, 1947, at Abinger
Authors: Jones H. Spencer
Published: February 2008

I enclose a list of the K‐indices of geomagnetic activity at Abinger for April to June, 1947, in Table 1.

In view of the interest which is now attached to “Sudden‐Commencement” phenomena, I append in Table 2 a list of the times at which these characteristic movements have appeared on the Abinger traces during the current year, to date [the time is “Universal Time” (UT= GMT)]. An asterisk (*) indicates that the movement, though abrupt, was not characteristically “sudden”.
Cheltenham K‐indices for January to June, 1947
Authors: Wiles William E.
Published: February 2008

Cheltenham K‐indices are submitted daily to the Washington Office of the United States Coast and Geodetic Survey and are currently being supplied in a weekly report to approximately the same agencies and investigators that formerly received the weekly “Report of Geomagnetic Activity” prepared by the Department of Terrestrial Magnetism, Carnegie Institution of Washington. In addition it is planned to publish quarterly tabulations of the Cheltenham K‐indices in this JOURNAL.

K‐indices are regularly scaled at all five of the standard observatories of the United States Coast and Geodetic Survey; monthly tabulations of these figures are filed in the Washington Office.
Recent geomagnetic data from observatories and stations in Japan
Authors: Wadachi K.
Published: February 2008

The geomagnetic data listed in Tables 1 and 2 are taken from the “Preliminary report of magnetic weather data from magnetic observatories and weather stations” supplied to the Commanding Officer, Headquarters 43d Weather Wing, in Tokyo.
Sitka Magnetic Observatory April to June, 1947
Authors: Campbell Joel B.
Published: February 2008

(Latitude 57° 03′.0 N., longitude 130° 20′.1 or 9h 01m.3 W. of Gr.)

April 8–9—A moderately disturbed period began abruptly at 21h 51m GMT, April 8. For the first 9.5 hours there was but little activity; however, at 07h 20m, April 9, both H and Z began to decrease. By 08h 17m H had decreased about 735 gammas. Both elements remained abnormally low until about 12h, April 9, when they gradually recovered to their normal values. It may be said that the disturbance ended at about 12h, April 9, but minor disturbances were recorded for several days following. K‐indices of 8 and 7 were recorded between 06h and 12h, April 9.
Alibag Magnetic Observatory April to June, 1947
Authors: Rao M. P.
Published: February 2008

(Latitude 18° 38′.3 N., longitude 72° 52′.3 or 4h 51m.5 E. of Gr.)

April 17–18—A sudden‐commencement storm of great intensity with an increase of 62 gammas in H, a decrease of 20 gammas in Z and an increase in westerly declination of 1′.5 (all in about three minutes) began at 12h 24m GMT, April 17. After a period of moderate intensity lasting for about seven hours, H fell rapidly at 19h 38m until 21h 35m when the minimum was reached. Thereafter H increased rapidly and began to fluctuate. The storm ended at about 22h 30m, April 18, recording two K‐indices of 8 for the successive intervals 18h‐24h, April 17, and four K‐indices of 6. Ranges: D, 9′.8; H, 429 gammas; Z, 103 gammas.
Huancayo Magnetic Observatory April to June, 1947
Authors: Ledig Paul G.
Published: February 2008

(Latitude 12° 02′.7 S., longitude 76° 20′.4 or 5h 0lm.4 W. of Gr.)

April 8—There was a sudden increase in H of 115 gammas in three minutes beginning at 21h 50m GMT, April 8, which was followed by a slow, large decrease with several slow, moderate peaks and bays during the night hours, but no real magnetic disturbance. D and Z were practically unaffected.
Note on “Sudden commencements” and other small characteristic impulses
Authors: Newton H. W.
Published: February 2008

The recent publication by the United States Coast and Geodetic Survey of a first instalment of ¼‐size reproductions of daily magnetograms, January to June, 1946, from the Cheltenham Magnetic Observatory, provides some interesting data in connection with “Sudden Commencements” (SC) and other small trace‐movements that are being studied at Greenwich. In a paper dated August, 1946, from the Royal Observatory, certain unexpected characteristics of SC‐occurrence were derived from the Greenwich data 1879–1944.

for two of the results given by the Greenwich analysis, the Cheltenham magnetograms provide a valuable comparison even for the short epoch of six months—a specially active six months, however, embracing some unusual solar phenomena.
Some experimental results obtained by ionospheric investigations in Sweden during the total solar eclipse of July 9, 1945
Authors: Gejer Sven , Åkerlind Per
Published: February 2008

Summary—Determinations of critical frequencies and virtual height made by the Swedish Board of Telegraphs are described and also other measurements made in Sweden during the eclipse.

Definite effects on the critical frequencies for the different layers were established by means of multifrequency recordings made at Östersund and Enköping. Thus the decrease in E‐layer electronic density from the assumed undisturbed value was about 57 per cent. For the F1‐layer the corresponding decrease was 63 per cent and for the F2‐layer approximately 33 per cent.
Cheltenham K‐indices for July to September, 1947
Authors: Wiles William E.
Published: February 2008

In continuation of data on geomagnetic activity in the last issue of the JOURNAL [52, 403–409 (1947)], the K‐indices for July to September, 1947, are given in Table 1 as determined from the records at the Cheltenham Magnetic Observatory.
International Association of Terrestrial Magnetism and Electricity
Authors: Joyce J. W.
Published: February 2008

Circular Letter No. 1, concerning plans for the Eighth General Assembly of the International Union of Geodesy and Geophysics to be held at Oslo, Norway, 17–28 August 1948.

(I) The time and place—After long postponement caused by the exigencies of War, the Eighth General Assembly of the International Union of Geodesy and Geophysics will be held during August, 1948, in Oslo, Norway. The Norwegian Committee in Charge of Arrangements has set tentative dates of August 17–28, 1948, for the meetings. The first two days will be devoted to administrative and organizational matters.
Cheltenham Magnetic Observatory July to September, 1947
Authors: Wiles William E.
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5, or 5h 07m.4 W. of Gr.)

July 17–20—A moderately severe magnetic storm began with a sudden commencement in all three elements at 17h 49m GMT, July 17, the severest part of the storm occurring within the first eight hours. Initial H‐motion was rapid and of large amplitude. After soon reaching a low value of 18,1777γ at 18h 06m, H then increased 265γ in a rapid although erratic manner until 20h 22m. After about 03h, July 18, H exhibited rapid pulsations of moderate amplitude. After 03h, July 19, long‐period motion of comparatively small amplitude predominated until the end of the storm at 17h July 20. Minimum H of 18,074γ occurred at 14h 36m, July 18. Following the sudden commencement Z decreased until 18h 01m, after which a rapid steady increase set in until 00h 08m, July 18, a change of 288γ being recorded. Z then decreased until 04h, when normal values were resumed. Z showed a rather rapid rise between 16h and 20h, July 18, and was erratic between 01h and 07h, July 19.
Comparative correlations of ƒ°F2 with “Ionospheric sunspot‐number” and ordinary sunspot‐number
Authors: Phillips M. Lindeman
Published: February 2008

Comparison was made between the correlation of monthly‐average ƒ°F2 at several ionospheric stations with monthly‐average Wolf relative sunspot‐number as compiled at Zurich, and with a new index of solar activity which has been provisionally called the “ionospheric sunspot‐number.” This quantity is derived from the ƒ°F2 observed at Washington, D.C.; Huancayo (Peru) and Watheroo (Western Australia)—stations having the longest time series of such data—for the hours 10 through 14 local time, using the well‐established trends of ƒ°F2 with sunspot‐number for these times and places. The average of correlation‐coefficients between smoothed annual sunspot‐number and monthly average of ƒ°F2 at noon for these stations for June, September, and December is 0.94.

The stations for which comparative correlations were made were not those whose data were used in deriving this so‐called “ionospheric sunspot‐number”, but others, having a series of ƒ°F2‐data extending over nearly as long a period of time. The correlation‐coefficients for these are given in Table 1.
Cheltenham K‐indices for October to December, 1947
Authors: Gebhardt Robert G.
Published: February 2008

In continuation of data on geomagnetic activity at the Cheltenham Magnetic Observatory [see Terr. Mag., 52, 403–409 and 522 (1947)], the K‐indices for October to December, 1947, as determined from the photographic records, are given in Table 1.
Temperature in the ionosphere
Authors: Petrie W.
Published: February 2008

In a recent paper, “Critical Survey of Recent Theoretical Work on the Ionosphere” by Pande [Terr. Mag., 52, 375–396 (1947)], the author discusses a number of the many papers dealing with the temperature of the upper atmosphere. He indicates that a good deal of confusion exists regarding the meaning of the word temperature in this case.
Witteveen Magnetic Observatory October to December, 1947
Authors: van Lohuizen H. P. Th.
Published: February 2008

(Latitude 52° 48′.8 N., longitude 6° 40′.1 or 0h 26m.7 E. of Gr.)

October 1–3—This period of magnetic activity with only temporarily moderate disturbances had started suddenly at 18h 09m, September 30. Activity was strongest between 14h 50m, October 2, and 6h, October 3. On all three days a K‐index of 5 was noted for the first 3‐hour‐interval, while between 12h and 24h, October 2, one K‐index of 6 and three K‐indices of 5 occurred.
Alibag Magnetic Observatory October to December, 1947
Authors: Rao M. P.
Published: February 2008

(Latitude 18° 38′,3 N., longitude 72° 52′.3 or 4h 51m.5 E. of Gr.)

September 30‐October 3—A moderate storm commenced suddenly at 18h 10m GMT, September 30, with an increase of 23 γ in H, a decrease of 5 γ in Z, and an increase of 0′.5 in westerly D. After a period of slight intensity lasting for about ten hours all the three elements recorded some large fluctuations till about 12h, October 1. The storm ended at about 04h 30m, October 3, giving five K‐indices of 5. Ranges: H, 224 γ; Z, 86 γ; D 8′.2.
Final relative sunspot‐numbers for 1947
Authors: Waldmeier M.
Published: February 2008

Table 1 contains the final sunspot‐numbers for 1947 for the whole disk of the Sun, based on observations made at the Zurich Observatory, supplemented by series furnished by other co‐operating observatories. Table 2 gives the number of spot‐groups on each day for the year 1947. The yearly mean of the group‐numbers is 13.4, against 7.8 in 1946. The yearly mean of the relative numbers is 151.6, against 92.6 in 1946.
Factors controlling the atmospheric conductivity at the Huancayo Magnetic Observatory
Authors: Parkinson W. D.
Published: February 2008

Some of the results of four months, recordings of atmospheric‐electric elements at Huancayo are presented. Positive small‐ion mobility appears to be constant, whereas negative small‐ion mobility has a regular diurnal variation. Positive small‐ion density is found to follow the normal equation of small‐ion balance. Values of combination‐coefficients are deduced.

A mechanism for the origin of variations in conductivity has been suggested by Gish. In general the results in this paper are in agreement with this suggestion. In the case of intermediate ions, a daily variation in mobility‐distribution is found, which suggests a source of intermediate ions close to the place of measurement.
Cheltenham Magnetic Observatory April to June, 1948
Authors: Ledig Paul G.
Published: February 2008

(Latitude 38° 44′.0 N., longitude 76° 50′.5 or 5h 07m.4 W. of Gr.)

April 7—A moderate magnetic disturbance began with a sudden increase in H at 03h 58m GMT, which was followed by relative magnetic calm until 16h 52m when there was recorded an hour and a half of increased value with rapid movements in H but affecting D in only a minor degree. Another period of calm began suddenly at 18h 21m followed by another increase with relatively large rapid movements in H at 19h 26m and lasting for a little over two hours, and then recording with only minor irregular movements from 22h 40m for the rest of the day. The K‐index for 18h to 21h was 6.
Zô‐Sè Observatory April to June, 1948
Authors: Burgard M.
Published: February 2008

(Latitude 31° 05′.8 N., longitude 121° 11′.2 or 8h 04m 45s E. of Gr.)

April 6–7—Abrupt beginning at 03h 58m (H = 36 γ), was followed by small activity. New sudden commencement at 16h 50m. A drop of H‐curve by 70 γ in three minutes took place at 18h 15m. Agitation was over April 8, in the morning.
Watheroo Magnetic Observatory April to June, 1948
Authors: Wood F. W.
Published: February 2008

(Latitude 30° 19′.1 S., longitude 115° 52′.6 or 7h 43m.5 E. of Gr.)

No magnetic storms of any consequence were recorded at Watheroo during April, May, and June, 1948.
Hermanus Magnetic Observatory April to June, 1948
Authors: van Wijk A. M.
Published: February 2008

(Latitude 34° 25′.2 S., longitude 19° 13′.5 or 1h 16m.9 E. of Gr.)

April 1— Following a period of moderate activity between 00h and 09h GMT, April 1, the traces remained slightly disturbed for several days.
A new magnetic survey of the Netherlands
Authors: Veldkamp J.
Published: February 2008

Summary—New magnetic charts of the Netherlands are given, based on measurements during the years 1942 to 1947 at 378 stations. The charts have been drawn for the epoch 1945.0. A chart of the anomalies in vertical and horizontal intensity shows regional disturbances which correspond to the tectonic structure of the crystalline base.
Cheltenham K‐indices for July to September, 1948
Authors: Ledig Paul G.
Published: February 2008

In continuation of data on geomagnetic activity at the Cheltenham Magnetic Observatory [see Terr. Mag., 52, 403–409 and 522 (1947), and 53, 166–167 (1948)] the K‐indices for July to September, 1948, as determined from the photographic records, are given in Table 1.
International Council of Scientific Unions, Mixed Commission on the Ionosphere
Authors: Beynon W. J. G.
Published: February 2008

The first meeting of the above Mixed Commission on the Ionosphere of the International Council of Scientific Unions was held at Brussels, July 28–30,1948. The following were present: Sir Edward Appleton (Chairman); Professor S. Chapman; Professor L. Vegard; Dr. R. v. d. R. Woolley; Dr. C. R. Burrows (representing Dr. J. H. Dellinger) ; Dr. M. A. Tuve (representing Dr. L. V. Berkner); Professor F. J. M. Stratton (Secretary, ICSU); Colonel E. Herbays (Secretary, URSI); Dr. W. J. G. Beynon (Secretary, Mixed Commission); Professor Manneback (Louvain University); Colonel Dorsiment (Vice‐President, URSI); Dr. M. Nicolet (Institut Royal Météorologie de Belgique); and M. Bourgeois (Directeur de l'Observatoire Royal de Belgique).

Six sessions of the Commission were held. The subdivision of the field of work and the introductory speakers are given below.
Selected days, preliminary mean K‐indices and C‐numbers for second quarter, 1948
Authors: Eaton Norma F.
Published: February 2008

The Table on page 478 gives mean K‐indices from the reports from 26 observatories and character‐figures, C, from 31. The quiet and disturbed days were selected in accordance with the method outlined on pages 219–227 in the December, 1943, issue of this Journal except that the daily indices B are no longer available. The method is a preferential selection based upon the C‐numbers, the sums of the eight daily mean K‐indices, the greatest daily K‐index, and the sums of the squares of the eight daily mean K‐indices.
Value of vertical component at De Bilt for 1906
Authors: Veldkamp J.
Published: February 2008

In your interesting list of geomagnetic observatories and annual values (VIII) corrected figures are given for the annual values of I, Z, and F (1899–1911) at De Bilt. I should like to remark that the annual value of Z for the year 1906 seems to be too high. This becomes clear if the secular changes at Greenwich, De Bilt, and Potsdam are compared. Presumably the base‐line of Z has been drawn very inaccurately in 1906, the year before Dr. van Dijk took charge of the absolute measurements. It is, however, not possible to correct the measurements and computations of the year in question, but the annual value of Z seems to me at least 100 γ too high.
College Magnetic Observatory July to September, 1948
Authors: Cleven Merril L.
Published: February 2008

(Latitude 64° 51′.9 N., longitude 147° 49′.3 or 9h 51m.3 W. of Gr.)

August 7–10—A moderate magnetic storm began sharply at 23h 00m GMT, August 7. The storm was characterized by short‐period, small‐amplitude oscillations superimposed upon large bays. The most severe part of the storm occurred between 16h and 19h, August 10, and consisted of large‐amplitude, short‐period oscillations. After 19h, August 10, the storm gradually died out; disturbed conditions, however, continued for about two days.
Sitka Magnetic Observatory July to September, 1948
Authors: Campbell Joel B.
Published: February 2008

(Latitude 57° 03′.0 N., longitude 135° 20′.1 or 9h 01m.3 W. of Gr.)

July 29–31—Rather large bays occurred between 09h and 13h GMT, July 29, and between 10h and 13h, July 31. The first bay produced K‐indices of 6 and 7 while the second produced a K‐index of 7.
Witteveen Magnetic Observatory April to September, 1948
Authors: van Lohuixen H. P. Th.
Published: February 2008

(Latitude 52° 48′.8 N., longitude 6° 40′.1 or 0h 26m.7 E. of Gr.)

April 6—After a sudden commencement at 03h 58m GMT, there was only very slight disturbance until 16h 52m, when a new disturbance started suddenly. One K‐index of 5 occurred in the interval between 18h and 21h. After 21h there was a long period of slightly disturbed conditions.
Apia Observatory July to September, 1948
Authors: Gerard V. B.
Published: February 2008

(Latitude 13° 48′.4 N., longitude 171° 46′.5 or 11h 27m.1 W. of Gr.)

August 7–11—A sudden commencement of 22 gammas in H at 23h 00m GMT, August 7, introduced a severe magnetic storm lasting until August 11. Following the sudden commencement a steady decline in H commenced, superimposed by rapid, irregular oscillations of small amplitude. At about 06h, August 8, H commenced to fall more rapidly and reached a minimum at 08h 52m. The range in H from the peak of the sudden commencement to this minimum was 346 gammas.
The Earth's magnetic and electrical moment
Authors: Eckersley T. L.
Published: February 2008

There are two outstanding problems. One is to explain the Earth's magnetic moment, and the other is to explain its electrical moment. Together with these, we have to explain the magnetic moments of all the astronomical bodies, such as the Sun and stars.

My feeling is that the two problems are connected. The Earth, for example, is very hot inside, and in the interior its temperature is above the melting point of iron. Such a hot body is like a hot filament, and produces an atmosphere of electrons. This atmosphere flows out to infinity and produces a space‐charge.
On electric currents induced by rotating magnets, and their application to some phenomena of terrestrial magnetism
Authors: Schuster Arthur
Published: February 2008

Speculative theories on the magnetic and electric relationship between the Sun and Earth lack all solid basis, until we can give an answer to the question, whether interplanetary space is to be considered an electric conductor or not. The question is not one which can at present be touched by any argument as to the possible amount of matter which space may contain, for the behavior of gases in our vacuum tubes is so much affected by the dimensions of the electrodes and of the vessel, that no conclusions can be drawn as to the electric behavior of molecules flying about in a boundless enclosure.

It is my purpose to show how the behavior of the magnetic needle on the surface of the Earth may give us some information on the point. If it fails to do so it will be because the conductivity of space falls below a certain assignable value, and even that knowledge will be a gain.
Ueber Simultan‐Beobachtungen erdmagnetischer Variationen
Authors: Eschenhagen M.
Published: February 2008

Als ein hervorragendes Ergebniss der ersten erdmagnetischen Forschungen Alexander v. Humboldt's und Arago's, sowie insbesondere der Beobachtungen des von Gauss und Weber begründeten magnetischen Vereins kann die Ermittelung der Gleichzeitigkeit des Auftretens gewisser starker Bewegungen der Magnetnadel an verschiedenen Orten gelten, und die magnetischen Termincurven in den Tafeln der “Resultate des magnetischen Vereins” fesseln noch heute wie damals das Auge durch das “Erkennen von Mass und Harmonie im anscheinend Regelosen.”

Als im Jahre 1882–83 im System der internationalen Polarforschung diese Terminbeobachtungen von neuem in bedeutendem Umfange angestellt wurden, ergab sich zwar auch für verhältnissmässig nahe, z. B. für die europäischen Stationen, ein gleiches Resultat wie früher, während die ferneren und namentlich die den magnetischen Polen näheren Stationen erkennen lassen, dass wohl ein etwa gleichzeitiges Auftreten der magnetischen Störungen stattfindet, dass aber ein unmittelbarer Vergleich einzelner erdmagnetischer Componenten nicht mehr möglich ist, sondern dass diese plötzlichen Variationen einem komplicirteren Gesetze gehorchen. Bei der Schwierigkeit, das umfangreiche Material, welches durch jene Terminbeobachtungen gewonnen ist, zu bewältigen, scheint es uns von Vortheil, erst mit einer einfacheren Frage zu beginnen und nicht die grossen, verhältnissmässig selten auftretenden Störungen, sondern die allerkleinsten, ziemlich häufig vorhandenen Bewegungen der Magnetnadeln zum Gegenstande des Studiums zu machen. Eine Trennung der Störungen in Gruppen—wobei man zunächst an eine Eintheilung nach der verschiedenen Grosse denkt—scheint nämlich zu dem Zwecke geboten, um zu erforschen, ob alle demselben Gesetze gehorchen, sich also z. B. nach Weltzeit richten, oder ob es Erscheinungen darunter giebt, die örtlicher Natur, wie z. B. die tägliche periodische Schwankung, oder die Einflüsse der Gewitter sind.
Logarithmen der Kugelfunctionen der ersten fünf ordnungen von fünf zu fünf grad
Authors: Schmidt Adolph
Published: February 2008

In der von mir im ersten Hefte dieser Zeitschrift mitgeteilten Untersuchung habe ich (S. 20) anstatt der gewöhnlich benutzten Kugelfunctionen gewisse Vielfache davon angewendet, die ich Rnm nannte und durch die Gleichungen

urn:x-wiley:02727528:media:tem222:tem222-math-0001
mit
definierte. Die Vereinfachung, die bei der dort behandelten Aufgabe die analytische Entwickelung dadurch erfuhr (wobei übrigens der Factor (2n + I) ohne Bedeutung war), hätte nicht hingereicht, die Abweichung von den üblichen Bezeichnungsweisen zu rechtfertigen. Was mich bereits an einer anderen Stelle zur Einftührung der Functionen Rnm veranlasste und was mich ihre allgemeine Verwendung hier befürworten lässt, ist der Vorteil, den sie in numerischen Entwickelungen gewähren.
Die Magnetischen Störungen der Jahre 1890–95, nach den Aufzeichnungen des Magnetographen in Potsdam
Authors: Lüdeling G.
Published: February 2008

In den “Ergebnissen der magnetischen Beobachtungen in Potsdam in den Jahren 1890 und 1891” (Veröffentl. des Kgl. Preuss. Meteorolog. Instituts, Berlin 1894) giebt Herr Eschenhagen eine Classification der magnetischen Curven, nach welcher er 5 verschiedene Arten unterscheidet, und zwar bezeichnet er mit

Character 1: Sehr ruhige Curven, die höchstens vereinzelte, sehr kleine Ausbuchtungen zeigen;

Character 2: Curven mit ziemlich ruhigem Verlauf; das Gesammtbild der täglichen Periode wird durch etwas häufigere, kleine Wellen nicht beeinträchtigt ;

Character 3: Leicht gestörte Curven, in denen secundäre Wellen von massiger Amplitude und kurzer Dauer (1–3 Stunden) auftreten, doch ist der tägliche Gang noch sicher erkennbar ;

Character 4: Ziemlich gestörte Curven, deren Gesammtbilder durch secundäre Wellen von grösserer Amplitude längere Zeit hindurch (6–8 Stunden) erheblich beeinträchtigt werden ;

Character 5: Curven mit sehr grossen, spitzen Wellen und Zacken, die in grosser Zahl und längerer Dauer auftreten und das normale Bild der Curven vollständig entstellen.
Isonomales et variations séculaires des composantes Y et X de la force magnétique horizontale pour l'époque 1857
Authors: de Tillo A.
Published: February 2008

Pour rendre complète la série des cartes des isanomales et des variations séculaires de magnétisme terrestre je viens de construire les quatre cartes ci‐jointes qui se rapportent à la composante occidentale—Y—et à la composante nord —X— de la force horizontale.

C'est seulement grâce au concours de M. le docteur Adolphe Schmidt de Gotha que j'ai pu exécuter ce travail, car jusqu'à ce jour je n'avais à ma disposition pour les composantes en question que les valeurs se rapportant à l'époque de 1829 consignées dans l'ouvrage de MM. Ermann et Petersen. Les valeurs calculées par Monsieur A. Schmidt correspondent à l'époque de l'an 1885; elles sont basées sur l'Atlas de magnétisme terrestre de M. Neumayer.
The electrification of the atmosphere
Authors: McAdie Alexander
Published: February 2008

Will the twentieth century number among its triumphs a complete electrical survey of the atmosphere? There are some good grounds for believing that it will.

In the first place, the subject of atmospheric electricity, unlike the commercial problems in electricity, has not been attacked by an army of workers; swarming on each new phase and forcing further development by tireless industry and determined zeal. The appearance of three such papers as are referred to below indicates a quickening and wide‐spread interest in the subject. Secondly, although we still lack a guiding theory as to the origin of the earth's negative charge, valuable data are accumulating so rapidly, and are now so accessible, that erroneous hypotheses may be quickly and effectively put to the test and disposed of. And thirdly, in the matter of instrumental equipment, we know the weakness of our present methods and apparatus, and also understand that where so many independent variables are to be dealt with, care must be taken to properly evaluate the electrometer readings. Furthermore, as with problems in meteorology, we must reach out from the individual observations to a series of similar simultaneous ones. The general laws of the potential variation in free air will be forthcoming when the necessary observations are made at many places. It is as logical for one to use a single thermometer to foretell marked temperature changes as to use a quadrant electrometer, and hope to determine from a series of isolated readings much of value concerning the potential of the air.
Secular variation expressions of the magnetic inclination
Authors: Littlehales G. W.
Published: February 2008

These expressions for the secular variation of the magnetic inclination at various important maritime stations have been deduced with a view of providing for the computation of the rate of change at a station at any time within the period of observation, and of bringing forward, from one epoch to another, values of the inclination observed in the regions were the stations are situated.

They have been used in this manner in connection with the preparation of the chart of the world, lately published by the Hydrographic Office, showing the isoclinic lines for the epoch 1897.
A remarkable law
Authors: Bauer L. A.
Published: February 2008

Let d = the mean value for the year of the total diurnal range or amplitude of the magnetic declination, i = the diurnal range of the inclination I, ϕ = magnetic latitude, then will the following formulae give close approximations to d and i for any place where I is known:—

In proof of this see diagrams opposite, [ϕ is obtained from the well‐known formula, tan I = 2 tan ϕ. The test of the formulae is a severe one; for k was derived from but 12 stations—all of them in the northern hemisphere— while in the diagram 12 additional stations (of which about half are from the southern hemisphere) are represented. k1 was determined from only two stations, Dublin and Batavia, while in the diagram the comparison is made for stations far distant from D and B. The only marked departures for (2) are shown by Jan Mayen and St. Helena. It should be recalled that i is far more difficult of experimental determination than d. The constants will be re‐computed for different years in the sun‐spot cycle and for different seasons of the year. For this reason a tabular presentation is postponed.] (1) was found empirically and then deduced theoretically, thus : Let d H represent the component of the horizontal diurnal deflecting force at right angles to the mean direction of the horizontal needle, then is : tan ½ d= d H/ H. Assume that d H varies inversely as H, and substitute for H the approximate value,1) 0.330 cos ϕ. Similarly we get (2) if we substitute instead of H the total force, F = 0.330
. It would have been very difficult to find (2) empirically.