Smithsonian

Contributions to Astrophysics

VOLUME 5, NUMBER 8

AN ANNOTATED BIBLIOGRAPHY ON

INTERPLANETARY DUST

by PAUL W. HODGE, FRANCES W. WRIGHT, AND

DORRIT HOFFLEIT

SMITHSONIAN INSTITUTION

Washington, D.C.

1961
Publications of the Astrophysical Observatory

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For sale by the Superintendent of Documents, U.S. Government Printing Office

Washington 25, D.C. - Price 25 cents
An Annotated Bibliography on

Interplanetary Dust

BY PAUL W. HODGE,1 FRANCES W. WRIGHT,1 AND DORRIT HOFFLEIT3

This annotated bibliography presents a

compilation of references to significant papers

relating to the study of interplanetary dust.

Some references have been included from

Bibliography on Meteoritic Dust with Brief

Abstracts compiled by Hoffleit (Harvard College

Observatory Reprint Series n-43, 45 pp., 1952),

and now out of print.

In the selection of references from the

Hoffleit bibliography, we have attempted to

include all important papers as well as representative samples that are of special interest

for historical reasons.

In the selection of references published since

the appearance of the Hoffleit bibliography, we

have been guided by the main principles that

Hoffleit adopted for her compilation:

Three types of dust have been considered as meteoritic dust in the search for material: particles that enter

the upper atmosphere as minute dust particles (the

zodiacal light may be a source of such); dust products

of the disintegration of larger meteoroidal masses

during their passage through the atmosphere; and

possible pulverized remnants of meteorite-impacts.

In addition, we include some papers relating

to interplanetary dust outside the earth's

atmosphere.

As far as practicable, the titles of journals

appear in the original language of publication.

For maximum usefulness to the reader, however, titles of papers are given in English.

Papers written in a language other than

English are usually indicated by a parenthetical

note.

1

 Harvard College Observatory and Smithsonian Astropbyslcal Ob*

servatory, Cambridge, Mass.

•Maria Mitchell Observatory, Nantuckct, Mass., and Yale University Observatory, New Haven, Conn.

AHNERT, E.

1954. Preliminary report on attempts to detect meteoritic dust. Die Sterne,

vol. 30, pp. 36-38. (In German.)

The lack of nickel in the spherules collected by Thomsen (1953) casts doubt on

their interplanetary origin. Hoffmeister

has collected dust in the neighborhood of

factories and has found spherules (45 to

135jt in diameter) similar, at first glance, to

Thomsen's spherules, but nonmagnetic.

Collections from more isolated regions contained no spherules. Collections from snow

showed no spherules but did show irregular

particles, 15 percent of which were magnetic, with diameters of 100 to 200MALLEN, C. W.

1956. Influence of solar atomic emission on

the orbits of interplanetary particles. Observatory, vol. 76, pp.

101-103.

The author discusses the magnitude of

the collision effect and shows that the rate

at which particles approach the sun may be

greater than that indicated by calculations

based on the Poynting-Robertson effect.

He does not consider the influence of largescale solar magnetic fields.

ANGSTRSM, A.

1929. On the atmospheric transmission of

sun radiation and on dust in the

air. Geografiska Annaler, vol. 11,

p. 156ff.

The author studies the effect of dust on

measurements of the solar constant; he be86
86 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

lieves that dust of cosmic origin may be

characterized by particles of smaller size

than those of volcanic origin or of dust

brought by convection from the earth to

the atmosphere.

ANONYMOUS

1885. Meteoric dust. Sci. American, vol.

52, p. 83ff.

The complete article reads: "A metallic

substance in powder or small granules has

been sent to the Science News laboratory

for examination. It proves to be meteoric

dust, largely composed of iron, nickel, and

silica. Dr. Batchelder, of Pelham, N.H.,

who sent the specimen, states that he collected the dust on the walk in front of his

house after a smart thunder shower. It is

probable that large quantities of this material fall upon the earth, but remain unnoticed. Much of the iron found in soils is

due to precipitation from interstellar

spaces, the particles becoming entangled

in our atmosphere."

ANYZESKI, V.

1947. A conjecture on the nature of some

meteoritic matter. Pop. Astron.,

vol. 55, pp. 169-171.

The author suggests that some meteors

may be solid hydrogen or ice with inclusions

of ordinary meteoritic material. Some

bolides on entering the atmosphere may

have a thick coating of hydrogen that

might account for some trains and might

explain the "nebulous meteors."

ARAGO, D. F. J.

1857. A list of the principal recorded showers of cosmic dust. Astron. Populaire, vol. 4, p. 208ff.

ASTAPOVICH, I. S.

1958. Bolides and their dust trains. In

Meteoric phenomena in the earth's

atmosphere. State Publishing

House of Phys.-Math. literature,

Moscow. (In Russian.)

In Chapter 29 the author discusses

bolides and their dust trains, and gives

lists of bolides observed in the U.S.S.R.

Chapters 34 and 35 deal with meteoric

and cosmic dust in the earth's atmosphere,

and meteoric material on the earth's

surface. The author gives a review of work

done by others on meteoric and cosmic

dust in the earth's atmosphere and on

meteoric material on the earth's surface.

He concludes that more than 16,000 tons of

meteoric material fall on the earth each

year.

BARBIER, D.

1955. Variations in intensity of the zodiacal

light. M6m. Soc. Roy. Sci. Li6ge,

ser. 4., vol. 15, pp. 55-71. (In

French.)

The author describes his photoelectric

measurements in three colors of the intensity of the zodiacal light, and discusses

the variations of intensity and color with

time.

BARRINGER, D. B.

1909. Meteor crater in Northern Central

Arizona. Pamphlet, National

Academy of Sciences, 24 pp.

The author discusses small specks of

meteoritic material admixed with rock

fragments.

BEACH, A.

1942. The zodiacal light. Astron. Soc.

Pacific, Leaflet No. 155, 8 pp.

This is a historical note in popular style.

BEARD, D. B.

1959. Interplanetary dust distribution.

Astrophys. Journ., vol. 129, pp.

496-506.

The author maintains that the most

reliable estimates of the concentration of

of interplanetary dust depend upon our

interpretations of measurements of

scattered light observed in the solar corona

and in the night sky. On this basis, and

also from a theoretical discussion, he concludes that interplanetary dust is probably

distributed as r~

3/a

, where r is the distance

from the sun, and certainly the variation
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 87

of the dust concentration with solar

distance has this rate as an upper limit.

He gives a few microns as the minimum

radius of the dust particles, and deduces

that near the minimum particle radius,

the particle number varies as a"3-

8

, where

a is the particle radius. The mass of all the

planets causes the dust to move towards

the ecliptic, and the distance from the

ecliptic is proportional to the solar distance

of the dust. The dust concentration at

the earth's orbit is approximately 10~M to

10~15 particles per cm3, but at the earth's

surface it is 10~10 to 10~" particles per cm3.

BEHR, A., and SIBDENTOPF, H.

1953a. Investigations of the zodiacal light

and the gegenschein from photoelectric measures on the Jungfraujoch. Zeitschr. Astrophys., vol. 32,

pp. 19-50. (In German.)

The authors observed the brightness and

the polarization of the evening zodiacal

light by using a photoelectric photometer

in two colors. They also observed the night

sky in the region of the gegenschein. They

interpreted the observations on the working hypothesis that the zodiacal light

material consists partly of free electrons,

which cause the observed polarization, and

partly of dust particles with radii greater

than 10"* cm, which cause no noticeable

polarization. For the space density of the

electrons near the earth the authors give

the value 600/cm3. The density rises in

the ecliptic to around 1000/cm3 at 0.6 a.u.

from the sun, and falls to about 120/cm3

at 1.3 a.u. from the sun. The space density

of dust particles in the ecliptic outside

Venus' orbit is constant, but inside Venus'

orbit falls off somewhat towards the sun.

The gegenschein has a simple explanation

if we accept the hypothesis that a cloud of

particles exists in the neighborhood of the

libration point of the sun-earth system.

Here the particle density exceeds by 10 or

102 the general particle density in the

ecliptic.

1953b. The structure of the zodiacal light.

Experimentia, vol. 9, pp. 134-135.

(In German.)

At the Jungfraujoch the authors made

photoelectric observations of the intensity

and polarization of the zodiacal light. Chi

the assumption that the polarization arises

from free electrons, the authors calculate a

space density of dust particles of 10~w/cm8,

which is nearly constant through the

ecliptic.

BOWEN, E. G.

1953. The influence of meteoric dust on

rainfall. Australian Journ. Phys.,

vol. 6, pp. 490-197.

Data on worldwide rainfall suggest a

correlation between rainfall and meteor

showers. In some localities heavy rainfalls

tend to occur on certain days in a pattern

repeated yearly. The author suggests that

meteoritic dust provides rain-forming nuclei when it enters cloud systems in the lower

atmosphere. Particles with diameters of

1 to 4/x require 30 to 50 days to fall to about

45,000 feet above the earth. This rate of

fall explains the 30-day lag between the

occurrence of the Geminid, Ursid, and

Quadrantid meteor showers, and the recorded maximum rainfalls. It is suggested

that noctilucent clouds originate from

meteoritic dust.

BRACEWELL, R. N.

1953. Meteors and rain. Observatory, vol.

73, pp. 249-250.

The author reports Bowen's findings on

meteors and rainfall.

BRIER, G. W. (see under Kline and Brier)

BULLRICH, K.

1949. Scattering of light on vapor and ice

particles. Zeitschr. f. Met., vol.

3, p. 335ff. (In German.)

The author discusses Link's attempt to

determine the extinction coefficient of the

air from measurements of light intensity at
88 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

the zenith. One difficulty is the uncertainty of the scattering function, which

varies with the composition of aerosols in

the atmosphere. The theoretical scatter

functions for water, dust, and ice, and for

various angles, are set up and compared

with various experimental determinations.

BURGER, J.

1949. Problems of cosmical aerodynamics.

Proceedings of symposium on the

motion of gaseous masses of cosmical dimensions, Int. Union Theoretical and Applied Mechanics and

Int. Astron. Union, edited by J.

Burger, 237 pp.

While meteoritic dust as such is not discussed, several of the papers on interstellar

matter have theoretical bearing, especially

papers by Spitzer, van de Hulst, and von

Weissacker.

CHLADNI, E. F. F.

1819. On fireballs and dust-falls. Vienna,

434 pp. (In German.)

Chapter 6 contains reports in chronological order of falls of dust or fine material

in dry or moist form. Also, pages 20-23

give a chronological table of supposed

meteoritic dust-falls between the years 472

and 1816. Most of these are described as

falls of red rain, red snow, or dust falls.

More than 50 examples are given.

CIALDEA, R.

1950. The spectral distribution of polarization in skylight. Ann. Geofis.,

vol. 3, pp. 357-370. (In Italian.)

From observations of the degree of polarization of light from the sky, three typical

conditions are indicated in which the polarization increases, remains constant, or

decreases with wave length. Theory shows

that this relationship depends upon the

ratio of scatter from particles of molecular

size to diffuse scatter from layers of large

particles, the thickness of these layers

determining the type of spectral distribution.

COSARI, D. L.

1834. Account of some remarkable hailstones which fell at Padua on the

26th of August, 1834. Ann. delle

Scienze del Regno Lomb. Veneto

(in Italian). See also Edinburgh

New Philosophical Journ., vol. 19,

p. 83ff. (in English).

Among the large and very numerous

hailstones found, a great number contained sandy matter. The author himself obtained only two such. In one there

was only a minute quantity at the center.

In the other, the nucleus of ash-grey color

was about % inch in diameter and surrounded by pure ice. The minute amount

of dust gained from this sample was insufficient for chemical analysis. Some of

the grains were easily attracted by a

magnet. It seemed probable that the dust

was a combination of iron or nickel with

some other unidentified substance.

CROZIER, W. D.

1956. Rate of deposit in New Mexico of

magnetic spherules from the atmosphere (Abstract). Bull. Amer.

Meteorol. Soc, vol. 37, p. 308.

This paper gives a condensed report of

the collections of magnetic spherules found

in New Mexico. The rate of deposit varies

only slowly, and may be correlated with

meteor showers. There are no rapid

changes in the rate of deposit which might

be correlated with short-period meteorological effects.

AND SEELY, B. K.

1949. Some techniques for sampling and

identifying participate matter in

the air. Technical Report No.

3-NR, Research and Development

Division, New Mexico School of

Mines, Socorro; Proceedings of the

First National Air Pollution Symposium, Pasadena. Abstracts: Pop.

Astron., vol. 57, p. 459, 1949; Sky

and Tel., vol. 9, p. 54, 1950.

Means have been developed for collection of air-borne particles of sizes down to
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 89

well below one micron. Methods are given

for combined microscopic and chemical

analysis. As a by-product of studies of

mass movements in the atmosphere, cosmic

dust in the air is being investigated. If

tests show iron, nickel, and cobalt, the dust

particles are probably of meteoric origin.

DAUBREE, A.

1893. Deep-sea deposits. Smithsonian annual report for year ending June 30,

1893, p. 545ff.

The paper includes a section on mineral

substances of extraterrestrial origin (pp.

557-560), gives general discussion on the

plausibility of finding meteoritic dust on

the sea-'bottom, and cites examples of

meteoritic dust accretion. In regard to the

friable chondritic meteorites that fell at

Orgueil on May 14, 1864, the author comments that if, instead of perfectly clear

weather, it had been rainy or the sky had

been only covered with clouds through

which the stones would have had to pass,

nothing could have been gathered up but a

viscous mud.

DAVIDSON, D. T. (see under Handy and Davidson).

DURST, C. S.

1935. Dust in the atmosphere. Journ. Roy.

Meteorol. Soc, vol. 61, pp. 81-87;

Discovery, vol. 16, pp. 87-88.

The paper gives a theoretical picture of a

dusty atmosphere in which each particle of

dust is surrounded by a pocket of air having

temperature and humidity different from

that of the general air mass. This picture

is corroborated by the rising of haze tops,

the air temperature above the Arabian Sea

during the S.W. monsoon, and the diurnal

variation of wind in that region. Some consequences are pointed out; one is that there

may be a layer of dust high up in the

atmosphere.

EHRENBERG, C. G.

1858. Meteoric dust from the Joshua Bates.

Monatsber. K. Akad. Wiss. Berlin,

pp. 1-10. (In German.)

The author discusses the great flame explosion near Baku, Feb. 7, 1839, and a fall

of black, polished, hollow kernels similar to

atmospheric iron dust found at the seabottom of the Pacific.

ELBERTY, W. T. (see under Stoiber, Lyons,

Elberty, and McCrehan).

FESENKOV, V. G.

1938a. On the origin of the zodiacal light.

Comptes Rendus, Moscow, new

sef., vol. 19, p. 677ff. (In French.)

1938b. On the role of galactic matter in the

phenomenon of the zodiacal light.

Comptes Rendus, Moscow, new

ser., vol. 19, p. 451ff. (In French.)

1938c. Some considerations of the origin of

the zodiacal light. Russian Astron.

Journ.,vol. 15, p. 368ff. (In French.)

1940. The problems of the zodiacal light.

Russian Astron. Journ., vol. 17, p.

25ff. (In Russian.)

1941. Investigation of the zodiacal light

based on observations in the tropics.

Russian Astron. Journ., vol. 18, p.

3Iff. (In Russian.)

1942a. The dynamic theory of the zodiacal

light. Russian Astron. Journ., vol.

19, pp. 28-49. (In Russian.)

1942b. Minor planets and cosmic dust.

Doklady Acad. Sci. Report, vol. 34,

pp. 163-167. (In Russian.)

1943. On the origin of the zodiacal light.

Doklady Acad. Sci. Report, vol. 39.

p. 377ff. (In Russian.)

1945. Cosmic material and the zodiacal

light. Meteoritika, vol. 2, p. 3ff.

(In Russian.)

1946. On the motion of meteoric dust in

interplanetary space. Russian Astron. Journ., vol. 23, pp> 353-366.

(In Russian with English abstract.)

The author discusses the influence of

gravity and radiation pressure.

1947. On the stability of the material of the

zodiacal light. Russian Astron.

Journ., vol. 24, pp. 39-43. (In

Russian.)
90 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

1949a. Atmospheric turbidity produced by

the fall of the Tunguska meteorite

on June 30, 1908. Meteoritika,

vol. 6, pp. 8-12. (In Russian.)

Unusual atmospheric phenomena that

occurred after the fall of the Tunguska

meteorite must have been caused by a

large mass of thinly scattered material in

the atmosphere. For shorter wavelengths

(4000 to 7000 angstroms) the atmospheric

transmission coefficients, determined at the

Mt. Wilson Station by the Smithsonian

Astrophysical Observatory, showed a noticeable decrease in atmospheric transparency from mid-July to mid-August,

1908, and some variation continued to

occur during the succeeding months. The

author estimates the particles from the

Tunguska meteorite to be of the order of

1/* in size, and the total mass to be at least

a few million tons.

1949b. The zodiacal light and the outer

atmosphere of the earth. Russian

Astron. Journ., vol. 26, p. 344.

Abstract in Astron. News Letter

(Harvard), No. 54, p. 3, 1951.

The author found an unsymmetrical

distribution of the zodiacal light, which he

believes is not of cosmic origin but originates in an unsymmetric extension of the

earth's atmosphere illuminated by the sun.

1950. On the gaseous tail of the earth.

Russian Astron. Journ., vol. 27,

p. 89. Abstract in Astron. News

Letter (Harvard), No. 51, p. 8.

The author announces the discovery of

"false zodiacal light" seen in the western

sky two or two and a half hours before

sunrise, and probably related to the

gegenschien. He discusses and rejects

Glyden and Moulton's meteoric hypothesis.

The density of "tail" decreases by a factor

of two at intervals of 4.67 radii of the

earth.

1958. Zodiacal light as the product of disintegration of asteroids. Russian

Astron. Journ., vol. 35, pp. 327-

334 (in Russian). An English translation appears in Soviet Astron.

Journ., vol. 2, pp. 303-309, 1958.

The disintegration of asteroids produces

a considerable amount of fine dust that

spreads into space. To explain the observed brightness of the zodiacal light, the

density of this dust in the neighborhood of

the earth must be 10"23 to 10~24 grams per

cm3, as a lower limit. Good agreement

exists between the observed form of the

zodiacal light and the theoretical isophotes

calculated (with the scattering fiinction of

Piaskovskaia-Fesenkova) from the known

distribution of inclination angles of asteroid

orbits. This fact constitutes the strongest

argument in support of a meteoritic or

asteroidal origin for the zodiacal light.

1959. On the nature of zodiacal light and

its probable connection with asteroids and periodic comets. Annales

d'Astrophys., vol. 22, pp. 820-838.

The author gives a mathematical discussion of the nature of the zodiacal light

and its probable relation to asteroids and

periodic comets. He shows that the observed characteristics of the zodiacal light,

including its polarization, can be accounted

for by the scattering of solar light by fine

interplanetary particles, if their properties

are similar to those of aerosols always present in the upper atmosphere. No observations support the hypothesis that light is

scattered by free electrons. It is possible

to obtain the theoretical isophotes of the

zodiacal light from the distribution of the

inclinations of the orbits of periodic comets

or asteroids. Periodic comets can account

for the observations, but an asteroidal

origin for the dust of the zodiacal light

would require velocities of several kilometers per second for the dust, with respect

to the parent asteroids.

FESSENKOFF, B.

1914. The zodiacal light. Gauthier-Villars,

Paris, 174 pp. (In French.)

FONTON, S. S. (see under Krinov and Fonton)
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 91

FREDERIKSSON, K.

1956. Cosmic spherules in deep-sea sediments. Nature , vol. 177, pp.

32-33.

Cores taken from the ocean bottom by

the Swedish Deep-Sea Expedition yielded

several hundred black spherules greater

than 35jt in diameter, composed of metallic

iron nuclei surrounded by magnetite. The

depth of the sedimentary layers in which

the spherules were found indicates a cosmic

origin. The estimated age of several million years for the sedimentary layers indicates that the spherules were probably

deposited in the Tertiary Period. Spherules obtained from atmospheric dust collected in Goteborg were found to be

industrial in origin.

FREE, E. E.

1911. The movement of soil material by the

wind. U.S. Dept. Agriculture,

Bureau Soils, Bull. 68, pp. 1-272.

This paper includes a bibliography of

Eolian geology, a discussion of extraterrestrial dust, numerous references to the

literature of cosmic dust, and a discussion

of volcanic dust.

GOODY, R. M. (see under Volz and Goody)

GOSSNER, J. L. (see under Whipple and Gossner)

GOTZ, F. W. P.

1948. Some investigations at the Arosa

Light-Climatic Observatory touching solar-terrestrial relationships.

Sixth Report of the Commission for

the Study of Relations between

Solar and Terrestrial Phenomena,

Orleans, p. 166.

"Bright nights" are probably associated

with an abnormal E-layer caused by invasion of cosmic dust particles.

GRIMMINGER, G.

1948. Probability that a meteorite will hit

or penetrate a body situated in the

vicinity of the earth. Journ. Applied Phys., vol. 19, pp. 947-956.

582933—61 2

The author considers particles down to

magnitude 30 (fine dust) and presents formulas for penetration if the particle speed is

high relative to the propagation of plastic

deformation in the target.

GUTH, V.

1955a. Meteoric astronomy. Bull. Astron.

Inst. Czechoslovakia, vol. 6, pp.

65-70 (in Russian); pp. 70-76 (in

English); the abstract covers pp.

75-76.

The author reviews Czechoslovakian

work on meteoritic dust during the period

1949 to 1955.

1955b. Meteoritic dust. Transactions of the

Int. Astron. Union, vol. 9, pp. 303-

304.

The author gives a short account of research on meteoritic dust. He states that

L. Kresak has disproved the observation of

F. Link (1953) and Z. Linkova that the intensity of the earth's shadow observed during lunar eclipses depends upon the amount

of meteoritic dust in the atmosphere;

Kresak has shown that only very big meteor showers could have any influence on

the intensity of the shadow. Guth states

that the question could be settled by optical measurements of the brightness and

polarization of the twilight sky.

HANDY, R. L., AND DAVIDSON, D. T.

1953. On the curious resemblance between

fly ash and meteoritic dust. Iowa

Acad. Sci., vol. 60, pp. 373-379.

The authors identify Thomsen's (1953)

spherules as fly ash from coal-dust furnaces.

HARTLEY, W. N., AND RAMAGE, H.

1901. The mineral constituents of dust and

soot from various sources. Proc.

Roy. Soc, London, vol. 68, pp.

97-109. See also abstract in Nature, vol. 63, p. 552, 1901.

The dust that fell November 16, 17,

1897, showed a regularity in composition

and a similarity to meteorites in being
92 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

magnetic and in having comparative freedom from extraneous matter. These

properties are in favor of its cosmic origin.

HASEGAWA, I.

1956. Collecting and theories of meteoric

dust. Tenkai (The heavens), Oriental Astron. Assoc. Memoir No. 175,

p. 226ff. (In Japanese.) Translation of some sections into English,

Reference Manual No. 1, Smithsonian Astrophys. Obs., pp. 1-46,

1959.

The author describes methods of collecting meteoric dust, gives details of various

collecting projects in Japan, and reviews

previous work by others. He is interested

primarily in magnetic spherules.

HAWKINS, G. S. (see under Whipple and

Hawkins)

HEARD, J. F.

1955. Meteorites large and small. Journ.

Roy. Astron. Soc, Canada, vol. 49,

pp. 49-63.

An investigation was made of dust collected by a filtering device operated in an

aircraft flying at an altitude of 6,000 feet

in the Arctic. About 300,000 cubic feet of

air were filtered, producing 1950 particles.

Examination under a microscope of 100-

power detected only two black spheres, in

contrast to 36 collected by the same

method above Windsor, Ontario, from air

subject to industrial pollution. This work

supports the conclusion of Hogg and Norris

in 1949 that such spherules have a terrestrial origin. No bright metallic splinters were found, and the black spheres are

probably not meteoritic. Assuming for

the particles a mean density of 3 gm/cm3,

the author computes that at 6,000 feet the

Arctic air contained about 7 x 10~8 gm/ft3

of solid material at the time of the collections. The magnetic fraction was 10 to

100 times greater than the amount expected

from van de Hulst's calculations, and

probably only a small fraction was extraterrestrial. The author favors the theory

that interplanetary dust is primordial

rather than debris from larger bodies, and

thinks that the study of micrometeorites

can hardly fail to add to our knowledge of

the origin and history of the solar system.

HEIS, E.

1859. The meteorite spherules of Captain

Callum. Wochenschr. Astron. Meteor. Geogr., new ser., vol. 2, p.

319ff. (In German.)

A shower of small black spherules like

very fine shot fell on the American ship

Joshua Bates, Nov. 14, 1856, about 60 miles

southeast of Java. A small quantity was

collected by Captain Callum for Lieutenant

Maury, who sent a sample to Ehrenberg for

microscopic study. Reported by Ehrenberg (1858). However, von Reichenbach

(1859) regards these spherules as evidence of a fireball.

HIRST, W. P.

1951. Some astronomical effects of radiation. Monthly Notes, Astron. Soc.

South Africa, vol. 10, pp. 44-46.

The author discusses the effect of the

sun's radiation on small bodies, comets,

and the zodiacal light.

HODGE, P.

1956. Opaque spherules in dust collected at

isolated sites. Nature, vol. 178,

pp. 1251-1252.

A preliminary report on dust collected

simultaneously at three widely separated

stations: in California, in central Alaska,

and in the Arctic. A detailed report appears in Hodge and Wildt (1958).

AND RlNEHART, J. S.

1958. High-altitude collection of extraterrestrial particulate matter. Astron.

Journ., vol. 63, p. 306. (Abstract.)

The authors describe dust collected by

millipore filters on jet aircraft flying at

heights ranging from 20,000 to 55,000

feet. The filters were examined with a

high-power microscope. About 10,000

particles were measured. Some dark

shiny metallic particles may be extra-
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST

terrestrial, since their abundance does not

change rapidly with altitude, as with

particles of terrestrial origin.

AND WILDT, R.

1958. A search for airborne particles of

meteoritic origin. Geochim. et

Cosmochim. Acta, vol. 14, pp.

126-133.

The authors report on results of a yearlong program involving daily collections of

atmospheric dust at several widely

separated, isolated sites. The particles are

opaque shiny spherules with diameters less

than 15/x, entirely different from the larger

spheres commonly found in densely populated areas. Their meteoritic origin is

suggested by recent evidence regarding

ablation of meteorites, and by the fact that

the rate of fall and the frequency distribution with size are the same at the several

stations. The average rate of fall at each

station was 1.1 spherules per cm2 per day

for particles greater than 3/z in diameter.

The rate of fall over the entire earth is

5X108 kg per year.

HOFFLEIT, D.

1949. Medal for meteor study awarded.

Sky and Tel., vol. 9, p. 32.

Note on F. L. Whipple's work on

micrometeorites.

1951. The Josiah and the Joshua Bates and

the meteoritic dust shower of

November 14, 1856. Pop. Astron.,

vol. 59, pp. 319-322.

The author clarifies the misconception

leading to the belief that there had been

two showers of dust, when in fact there had

been only one.

HOFFMEISTER, C.

1930. Contribution to the photometry of the

southern Milky Way and the

zodiacal light. Veroff. BerlinBabelsberg, vol. 8, pt. 2, 60 pp.

(In German.)

The author gives photographically determined isophotes for the zodiacal light.

1932. Investigation of the zodiacal light.

Veroff. Berlin-Babelsberg, vol. 10,

pt. 1, 141 pp. (In German.)

The author associates the zodiacal light

with the concept of very small minor

planets.

1934a. On the cometary disturbances of the

upper layers of the atmosphere.

Sitzungsber. Bayer. Akad. Wiss.,

Math-Nat. Abteil., pp. 129-144.

1934b. A hitherto unknown cosmic disturbance in the upper atmosphere. Naturwissenschaften, vol. 22, pp. 458-

460.

1934c. Luminous bands, ionization of the

upper atmospheric layers and propagation of electromagnetic waves.

Forsch. u. Forschr., vol. 10, pp.

322-323.

In the above three papers the author asserts that ionospheric disturbances as well

as luminous night-sky phenomena can with

a certain degree of assurance be attributed

to cosmic disturbances or to intrusions of

dust into the upper layers of the

atmosphere.

1934d. On the nature of the zodiacal light.

Pop. Astron., vol. 42, pp. 426-430.

1937. Meteors. Akademische Verlagsgesellschaft, Leipzig, chapters 2, and 3.

(In German.)

This book contains material on interstellar absorption, smoke trails, dust and

ionization, ionization from dust-clouds of

supposed cometary origin, the possibility

that meteors and cosmic dust clouds might

have influence on climate or weather, and

related topics.

1941. Remarks on the problem of the zodiacal light. Astron. Nachr., vol.

271, p. 204ff. (In German.)

The author attempts to clarify the

reasons for the differences between the

terrestrial theory of F. Schmid and other

theories.

1942. Remarks on the problem of the zodiacal light. Astron. Nachr., vol.

273, p. 131ff. (In German.)
94 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

1951a. Interplanetary matter. Naturwiss.,

vol. 38, p. 227S. (In French.)

A semipopular article.

1951b. Specific luminous phenomena in the

center of the ionosphere. Ergebnisse der exakten Naturwiss., vol.

24, p. Iff. (In German.)

The author describes observed phenomena and interprets them in terms of micrometeorites.

1955. On some peculiar aspects of the

zodiacal light. Mem. Soc. Roy.

Sci. Liege, ser. 4, vol. 15, pp. 72-79.

The author discusses some peculiar

aspects of the zodiacal light and the

gegenschein. He emphasizes that the zodiacal light is a topological or astrometric

problem, as well as a physical one.

HOGG, F. S.

1949. Meteoritic dust. Astron. Journ., vol.

54, p. 205. (Abstract.)

The author outlines a program for collecting atmospheric dust and for extending

the work to the Arctic.

1950. Graduate work in meteoritic astronomy and work on meteoritic dust

in Canada. Letter to Professor

Leonard, Pop. Astron., vol. 58,

pp. 357-358.

The author discusses the search for

meteoritic matter in atmospheric dust,

and dust collecting in the Arctic.

HOPPE, J., AND ZlMMERMANN, H.

1954. Separation of interplanetary from

industrial particles. Die Sterne,

vol. 30, pp. 33-36. (In German.)

The authors give a critical analysis of

Thomsen's (1953) work. They show pictures of spherules obtained from iron

filings that had been passed through the

flame of a Bunsen burner, of steel chips,

and of spherules produced by welding.

Collections made at various distances

from the center of Jena suggest that

Thomsen's spherules were industrial in

origin. The authors believe that some

extraterrestrial particles reach the earth's

surface but that identification would be

difficult.

HTTLBURT, E. O.

1930a. A theory of zodiacal light. Phys. Rev.,

ser. 2, vol. 35, p. 663. (Abstract.)

The paper presents a theory that assumes

that the zodiacal light originates in the

uppermost layer of the earth's atmosphere.

1930b. The zodiacal light and the gegenschein as phenomena of the earth's

atmosphere. Phys. Rev., ser. 2,

vol. 35, pp. 1098-1118.

HULST, H. C. VAN DE

1949. Scattering in the atmospheres of the

earth and the planets. In Kuiper,

ed., The atmospheres of the earth

and planets, pp. 49-111.

1955. On the polarization of the zodiacal

light. Mem. Soc. Roy. Sci. Liege,

ser. 4, vol. 15, pp. 89-95.

The author discusses the polarization of

the zodiacal light. He explains that, contrary to some claims, the polarization of

the dust component may be appreciable

and that an uncertainty in the electron

density arises from this fact.

JAGER, C. DE

1955. The capture of zodiacal dust by the

earth. Mem. Soc. Roy. Sci. Liege,

ser. 4, vol. 15, pp. 174-182.

The author discusses the capture of zodiacal dust by the earth. The amount of

extraterrestrial dust observed on the earth

is about 103 times greater than the amount

computed from meteor frequencies. The

author suggests that for the zodiacal dust

the capture diameter of the earth is approximately 8 x 106

 km. The daily deposit of dust was computed on the basis of

two different density distributions of the

zodiacal light. From van de Hulst's figures the author found 1.6 x 103

 kg per day,

and from Elsasser's he found 9.0 x 103 kg

per day.
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 95

JUNG, B.

1939. Investigations of the zodiacal light.

I: Gas and solid matter in the

solar system. Mitt. Univ. Sternwarte Breslau, vol. 5, p. 50ff. (In

German.)

The author discusses the motion of dust

particles in interplanetary space.

KAISER, T. R., AND SEATON, M. J.

1955. Interplanetary dust and physical processes in the earth's upper atmosphere. M6m. Soc. Roy. Sci. Liege,

ser. 4, vol. 15, pp. 48-54.

The authors conclude that the density

of interplanetary particles is too low for

them to have much effect on the physical

processes in the terrestrial upper atmosphere, but that the particles probably account for certain kinds of ionospheric

abnormalities.

KALLMAN, H. K.

1955. Quantitative estimate of frequency

and mass distribution of dust particles causing the zodiacal light

effect. M&n. Soc. Roy. Sci. Liege,

ser. 4, vol. 15, pp. 100-113.

The author gives a quantitative estimate of frequency and mass distribution

for dust particles that cause the zodiacal

light. She concludes that interstellar space

has two classes of dust particles, with different origins but similar densities: fastmoving meteor particles and a quiescent

interplanetary dust cloud.

KAMMERMAN, A.

1886. Meteor shower of Nov. 27, 1885.

Astron. Nachr., vol. 113, pp. 138-

140. (In German.)

This paper deals with Yung's analysis of

the dust that fell on and after November 27

at Gent. A considerable number of meteoritic particles were found.

KARANDIKAR, R. V.

1948. Effect of dust and haze on the spectral

distribution of zenith-scattered radiation. Proc. Indian Acad. Sciences, "A," vol. 28, pp. 46-53.

Spectrophotometric observations on

zenith-scattered light showed anomalous

behavior, which is attributed to scattering

by large particles present in the atmosphere.

KIZILIRMAK, A.

1954. Preliminary report on the amounts of

iron dust which daily fall on the

surface of the earth. Communications de la Faculty des Sciences de

l'Universit^ d'Ankara, vol. 6, ser.

A, Fasc. 2, pp. 186-192.

The author describes his collection of

irregular magnetic dust particles 1 to IOOJI

in length, found in and around Ankara.

Chemical analysis showed iron, but no

nickel, cobalt, nor magnesium. The number of iron particles that fell daily was recorded with the daily meteorological data.

The iron dust may be terrestrial, the result

of erosion; or it may be extraterrestrial,

from meteors. Some evidence indicates

that maximum particle counts occur on or

near the days of meteor showers.

KLINE, B., AND BRIER, G. W.

1958. A note on freezing nuclei anomalies.

Monthly Weather Review, vol. 86,

pp. 329-333.

The authors made daily observations of

freezing nuclei in the Washington, D.C.,

area during the first three months of 1958.

In spite of the probable observational uncertainties, the fluctuations in the number

of freezing nuclei were highly significant.

Near the January dates for which maxima

were predicted by a meteoric dust hypothesis the values were abnormally high,

but later peaks do not seem to be associated with any known major meteor

streams. An analysis of the dates of

marked peaks shown by similar observations made since 1954 at other places tends

to confirm the presence of singularities in

January which are statistically significant.
SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

KOLOMENSKY, V. D., AND YuDIN, I. A.

1958. The mineral composition of the fusion

crust of the Sikhote-Alin meteorite,

and meteoritic and meteoric dust.

Meteoritika, vol. 16, pp. 59-66.

(In Kussian.)

Sharp-edged particles from the dust contain nickel-iron, magnetite, and iron hydroxides (limonite and goethite). A few

spherical and rounded particles, both solid

and hollow, and from 0.2 to 0.04 mm in

size, resemble in mineral composition the

external zone of the fusion crust of the

larger meteorites, which consists mainly of

oxymagnetite. The latter has a microgranular structure with nodules of isometric form, 3 to 8/* in diameter.

KRASOVSKY, V. I.

1946. Cosmic rays and the optical concentration of scattered matter. Comptes Rendus, Acad. Sci., U.S.S.R.,

new ser., vol. 51, p. 183ff. (In

Russian.)

Accepting as fact that iron and other

metals in interstellar space have positive

charges while stony particles have negative

charges, the author computes that a cloud

of iron meteoritic particles of 10 a.u. radius

would have a potential of 3 x 1011 volts.

He then considers the charges that would

occur if the meteoritic cloud penetrated a

gas cloud. Charged particles with velocities greater than 45 km per sec would

release kinetic energy, possibly giving rise

to the emission of cosmic rays.

KRINOV, E. L.

1955. Basic meteoritics. State Publishing

House of Technical-Theoretical Literature, Moscow. (In Russian.)

Translated by Irene Vidziunas and

edited by Harrison Brown as Principles of meteoritics, Pergamon

Press, 535 pp., 1960.

The author describes dust found at the

site of fall of the Sikhote-Alin iron meteorite. He favors the following classification

for extraterrestrial material: meteoric, meteoritic, cosmic. (1) Meteoric dust results

from the disintegration of meteoric bodies

hi the atmosphere and comprises spheroidal

particles with diameters from a few microns

up to 100/i. (2) Meteoritic dust is the

product of the crushing of meteorites that

have fallen to the earth. The particles are

small, acute-angled, irregular, and have a

composition and microstructure identical

to those of meteorites. (3) Cosmic dust

includes the smallest particles that invade

the earth's atmosphere from interplanetary

space; because of their small mass they

reach the earth's surface practically unaltered. They are Whipple's "micrometeorites." From examination of particles at

the site of the Sikhote-Alin fall, the author

concludes that particles of the dust trains

of bolides are solidified globules that are

blown away from the melting surfaces of

meteoric bodies. He shows photographs

of magnetic particles collected from the

site. They comprise primarily meteoritic

dust, plus a small number of globules with

diameters of 3/u to 800/z, as well as small

hollow flasks with open necks, and dropshaped particles.

AND FONTON, S. S.

1952. Detection of meteoric dust at the

place of fall of the Sikhote-Alin iron

meteorite shower. Doklady Acad.

Sci. Report, vol. 85, pp. 1227-1230.

(In Russian.)

The particles of dust trains of bolides

seem to represent solidified droplet-globules

that are blown away from the melting surfaces of meteoric bodies as they move with

cosmic speeds and are spattered in the

earth's atmosphere. Traces of the melted

matter were found on the surfaces of the

Sikhote-Alin meteorites. Particles subjected to fusion or those formed by the

condensation of gasses may be spherules

and particles that are not affected by high

temperatures may be acute-angled.

1954. Meteoric dust from the place of fall

of the Sikhote-Alin iron meteorite

shower. Meteoritika, vol. 11, pp.

122-131. (In Russian.)

The authors present a table of the frequency of spherules and meteoritic particles
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 97

from samples of the soil at the SikhoteAlin site. For another presentation of the

work, see Krinov (1952).

KULIK, L. A.

1926. On the question of the relation between meteorites and comets.

MirovedSnie", vol. 15, p. 173ff. (In

German.)

The author discusses luminous night

clouds associated with the great Siberian

meteorite fall.

LAEVASTU, T., AND MELLIS, O.

1955. Extraterrestrial material in deep-sea

deposits. Trans. Amer. Geophys.

Union, vol. 36, pp. 385-389.

The authors examined black spherules

from a Pacific Ocean core obtained by the

Swedish Deep-Sea Expedition of 1947-

1948. They estimate that about 125 tons

of black cosmic spherules fall on the earth

each year and suggest that Pettersson and

Rotschi's (1952) chemical analysis gave too

large averages of NiO and Fe2O3 for the

minute quantities of spherules present.

The authors conclude that nickel and iron

seem to be derived partly from coprecipitation from sea water.

LANDSBERG, H. E.

1947. A report on dust collections made at

Mount Weather and Arlington,

Virginia, 1 October to 20 November, 1946. Pop. Astron., vol. 55,

pp. 322-325. (Abstract.)

Certain of the dust particles are thought

to be of cosmic origiD.

LANE, A. C.

1913. Meteor dust as a measure of geologic

time. Science, vol. 37, pp. 673-

674.

LARMOR, J.

1938. Origins of the zodiacal light. Nature,

vol. 141, p. 201ff.

As origin, the author suggests a nebula

surrounding the sun.

LEONARD, F. C.

1941. Small aerolites recovered from the

site of the Holbrook, Arizona, fall

of 1912. Pop. Astron., vol. 49,

pp. 384-386.

Aerolitic particles have been found in

ant-hills; they weigh from 0.0074 to 0.0628

gm.

LEVI-CIVITA, T.

1930. Maxwellian distribution of cosmic

dust. Pont. Ace. Sci., N. Lincei,

Atti, vol. 83, p. 176ff.

Cosmic dust includes particles of all

sizes, even meteorites. If the distribution

is Maxwellian, the result of an encounter

with a planet is always directly opposed to

the planet's motion.

LEVIN, B. J.

1943. The nature of gas and dust trains of

various types. Russian Astron.

Journ., vol. 20, p. 49ff. (In Russian.) See also, Doklady Acad.

Sci. Report, vol. 38, p. 304ff.

1955. Spatial density of interplanetary particles and their distribution according to size. Me"m. Soc. Roy. Sci.

LiSge, ser. 4, vol. 15, pp. 114-124.

(In French.)

The author discusses the space density of

interplanetary particles and their distribution in size. He concludes that at present

the astronomy of meteors and studies of

the zodiacal light and corona give only

uncertain data on the solid matter in

interplanetary space. However, the study

of interplanetary matter is important both

for astronomy and for the physical constitution of the earth. Hence, theoretical

and observational studies should be carried

out by all means at our disposal.

1956. Physical theory of meteors and meteoric material in the solar system.

Publishing House of the Academy

of Sciences, Moscow, pp. 266-281.

(In Russian.)

The author discusses the results obtained

by other investigators, and summarizes in
98 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

a table some values obtained by various

workers for the space density of meteoric

material in the vicinity of the earth's

orbit. He believes that a considerable

amount of meteoric material reaches the

earth's atmosphere not in the form of

cosmic dust, but in the form of large porous

bodies that disintegrate and evaporate in

the atmosphere.

LIBEDINSKY, B.

1933. Cosmic dust and noctilucent clouds.

Himmelswelt, vol. 43, p. 226ff. (In

German.)

This paper gives a general review and

reaches a good many forced conclusions.

It summarizes knowledge of noctilucent

clouds, the bright night clouds of June 30,

1908, and the Tunguska meteorite fall, and

attempts to show that the cosmic dust

cloud which produces the bright nights and

the noctilucent clouds has a period of about

6 years and is associated with the PonsWinnecke comet. It discusses Nordenskiold's description of meteoritic dust-fall.

LINK, F.

1950. Optical soundings of the upper atmosphere with the help of lunar

eclipses. Internat. Assoc. Terr.

Magn. Elect. Bull., no. 13, pp. 502-

503. (In French.)

Observations of the optical density of the

earth's shadow show it to be a function of

the distance from the center; and from

photometric theory the density of the

shadow can be calculated. The difference

between the observed and the computed

values increases rapidly from 24 km to the

top of the O8 layer. A further layer is

indicated at 100 km; it may be meteoric

dust.

1953. Meteoric dust in the earth's atmosphere. Bull. Astron. Inst. Czechoslovakia, vol. 4, pp. 158-161. (In

French.)

The author considers the possibility that

a high altitude layer of meteoritic dust

would cause absorption of light that could

be observed during lunar eclipses. For the

effective diameter of particles that produce

the greatest absorption he obtains values

of the order of one ft. A systematic, extensive collection of meteoric dust could

provide data on the nature of the particles

and their total mass. However, particles

that enter the earth's atmosphere simultaneously are not collected simultaneously

on the surface of the earth, since the time

required to fall depends on their diameters.

During a long time of fall, fine iron particles may be oxidized and therefore would

not be found in magnetic material collected.

1955. The role of meteoric dust in the earth's

atmosphere. M6m. Soc. Roy. Sci.

Li6ge, ser. 4, vol. 15, pp. 35-47.

(In French.)

The author summarizes previous observational and theoretical research on meteoric dust in the earth's atmosphere.

1956. On the amount of meteoric dust in the

earth's atmosphere. Bull. Astron.

Inst. Czechoslovakia, vol. 7, pp.

69-75. (In French.)

A difference of the order of 10 exists between values for the amount of meteoritic

accretion deduced by direct determinations

(Pettersson 1955) and by indirect measures

(Link 1953). To explain the difference

Svestka thought it necessary to postulate

meteoric particles with radii one tenth of a

micron or less, while the author suggested

a radius of one micron. Link believes

Svestka's arguments to be incorrect, and

that it is preferable to retain the value of

one micron and to look elsewhere for an explanation of the difference, if it is not

simply the result of the inevitable errors in

the methods employed.

LINKE, F.

1909-1910. Lectures: 2. Twilight phenomena, their regularities and disturbances. 3. Geophysical occurrences

during the earth's passage through

a comet's tail. 4. Preliminary geophysical results of observations of

the passage of the comet from May

18-19 in Frankfort on the Main.
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 99

Jahresbericht des Physikalischen

Vereins zu Frankfurt am Main,

pp. 55-60. (In German.)

This paper discusses normal effects at

twilight of dust in the atmosphere, the additional effects that might be anticipated

from the passage of Halley's comet, and

very briefly the effects actually observed.

1910. Aeronautical Meteorology, 126 pp.

The author mentions Halley's comet as a

source of atmospheric dust, May 1910 (pp.

40-45), and discusses the effect of sunlight on the diurnal variation of heights of

dust-layers in the atmosphere, and optical

phenomena from dust.

AND OTT, J.

1909-1910. Geophysical observations on the

Feldberg i.T. during the passage of

Halley's comet. Jahresbericht des

Physikalischen Vereins zu Frankfurt am Main, pp. 98-126. (In

German.)

Observations of Bishop's ring indicate

that dust penetrated deep into the atmosphere but settled into the lower regions

only gradually (a matter of days).

LOCK, C. (see under Packer and Lock)

LYONS, J. B. (see under Stoiber, Lyons, Elberty, and McCrehan)

LYTTLETON, R. A.

1948. On the origin of comets. Monthly

Notices Roy. Astron. Soc. London,

vol. 108, pp. 465^75.

During the passage of the sun through

a cloud of interstellar dust the particles

converge to the accretion-axis where their

transverse velocities are destroyed by collisions. A stream of dust forms at the

axis, and for low relative speed of the sun

and cloud, that part of the stream within

several hundred astronomical units is

captured and flows toward the sun.

1951. On the structure of comets and the

formation of tails. Monthly Notices Roy. Astron. Soc. London,

vol. Ill, pp. 268-277. See also

abstract in Observatory, vol. 71,

p. 179.

The author considers comets as consisting of widely separated solid particles, some

of which collide with one another at relative

velocities sufficient to pulverize them. The

resulting particles of diameter of the order

10"6 cm are repulsed by solar radiation

pressure to form the tails.

MAPPER, D. (see under Smales, Mapper, and

Wood)

MAYNE, K. I.

1956. Terrestria l helium. Geochim. et

Cosmochim. Acta, vol. 9, pp. 174-

182.

The amount of He4 released to the atmosphere from the earth's crust is 60 times

greater than had previously been estimated. Because of the isotopic abundance

ratio of atmospheric helium (He3/He*~1.2

X10~fl), the production of He3 in the atmosphere must be greater than the amount

calculated from (n, H3) reactions induced

by cosmic rays on nitrogen. Extraterrestrial dust, continuously received by the

earth at the rate of 5,000 tons per day,

is considered as a source of He3. The

author favors the theory that this is the

interplanetary dust associated with the

zodiacal light. He stresses the desirability

of cosmic dust collection, particularly in

Antarctica where one cubic meter of snow

should contain one milligram of cosmic

dust.

MCCREHAN, R. H. (see under Stoiber, Lyons,

Elberty, and McCrehan)

MELLIS, O. (see under Laevastu and Mellis)

MEUNIER, S.

1884. Dust, liquids, and gas of meteoritic

origin. Chemistry Encyclopedia,

II, Metalloids, pp. 307-318. (In

French.)

Treats various sources: earliest, Saloman,

Hanover, Dec. 3, 1586; latest, Yung,
100 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

Switzerland, 1876. Also states, "Le navier

Josiah-Bates naviguant, dans la nuit du 24

au 25 Janvier 1859." Cf. E. Heis (1859),

who gives different dates; 1859 is wrong.

1903. Shower of dust recently observed in

Iceland. Comptes Rendus, Paris,

vol. 136, p. 1713ff. (In French.)

Red snow was observed the evening of

May 27 at latitude 64°54' N, longitude

13°40' E, and opaque black granules, some

rounded, glassy, "des filaments et des

globules." Similar dust fell in Norway

and Sweden in 1875, and was like Batavian

tears. No polarization was observed.

Such material is probably produced suddenly at temperatures below —100°.

AND TlSSANDIER, G.

1878. The presence of magnetic spherules,

similar to those of atmospheric

dust, in rocks of ancient geological

periods. Comptes Rendus, Paris,

vol. 86, p. 450ff. (In French.)

Magnetic spherules collected from the

air and the sea-bottom are compared with

certain similar ones found in sands from

deep wells.

MILLMAN, P. M.

1954. Meteor showers and rainfall. Journ.

Roy. Astron. Soc. Canada, vol. 48,

pp. 226-227.

The theory that rainfall and meteor

showers are related confronts astronomical

and geophysical difficulties that have not

been fully considered. Rainfall data for

the southern hemisphere (Bowen, 1953)

cannot be correlated with meteor showers in

the northern hemisphere. The rate of

settling from the 100-km level will vary

greatly with the size of the meteoritic

particles, and relatively sharp rainfall peaks

are difficult to explain.

MINNAERT, M.

1955. Dust in the interplanetary space.

M6m. Soc. Roy. Sci. Liege, ser. 4,

vol. 15, pp. 15-34.

The author introduces a series of papers

on dust in interplanetary space, presented

at an international conference on Astrophysics, held at Liege in July 1954.

MURRAY, J., AND RENARD, A. V.

1884. On the microscopic characters of

volcanic ashes and cosmic dust, and

their distribution in the deep-sea

deposits. Proc. Roy. Soc. Edinburgh, vol. 12, p. 490ff.

NEWKIRK, G.

1959. Measuring variations in sky brightness. Naval Research Reviews,

October, pp. 20-22.

Preliminary measurements show that at

an altitude of 38,000 feet the daytime sky

is five times brighter than it would be if the

earth's atmosphere were free of contaminating dust. Measures were made by

means of a coronograph flown in a highaltitude balloon.

NININGER, H. H.

1941. Collecting small meteoritic particles.

Pop. Astron., vol. 49, pp. 159-162.

The author discusses the recovery of

gravel-size meteorites and the importance

of studying even finer dust.

NORDENSKISLD, N. A. E.

1874a. On the cosmic dust which falls on the

surface of the earth with the atmospheric precipitation. Philos. Mag.,

ser. 4, vol. 48, p. 546ff.

1874b. On cosmic dust which falls with atmospheric precipitation on to the earth's

surface. Poggendorf, Annalen der

Physik und Chemie, vol. 151,

pp. 154-165. (In German.)

The author believes he has proved the

presence of cosmic dust by comparison with

analyses of other dusts collected from air.

1883. Program for the expedition to Greenland. Nature, vol. 28, p. 37ff.

From the collection of new data on cosmic dust, the author believes there is

greater variation in dust falls than is generally assumed. The polar regions especially are suited to a search for such

material.
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 101

1885. Studies and research instigated during

my travel in the High North. Leipzig, Brockhaus. (In German.)

This paper is mostly devoted to the

author's theory of the vast importance of

cosmic dust and contains much about

meteors and meteorites as well as a list of

dust falls (p. 157). Pages 121-127 cover

the geological importance of the fall of

cosmic dust on the earth's surface with

special consideration of the theory of Kant

and Laplace.

1894. On the great dust fall in Sweden and

adjacent lands on May 3, 1892.

Met. Zeitschr., vol. 11, p. 212ff.

(In German.)

The subsections present older observations of dust-showers, the various types,

dust of unquestionable cosmic origin, lists

of falls, and analyses.

OLEAK, H.

1956-1957. The behavior of small meteoritic

particles in the earth's atmosphere.

Wiss. Zeitschr. Friedrich-Schiller

Universitat, Jena, vol. 6, pp. 133-

143. (In German.)

The author presents a mathematical discussion of the behavior of small meteoritic

particles (10~2 to 10~7 cm) in the atmosphere, and discusses their velocities as a

function of height, the height at which they

begin free fall, the time of fall, and problems of ablation.

OPIK, E. J.

1955. Cosmic sources of deep-sea deposits.

Nature, vol. 176, pp. 926-927.

The author gives a table (with references)

for various abundance ratios obtained for

iron, nickel, cobalt, and copper. He suggests that the nickel of the deep sea may be

of cosmic origin, even though other abundances in sea material differ from those

of meteorites. There is no good reason to

assume that abundances of elements in

cosmic dust would be identical with those

in meteorites. Attention is called to the

larger ratio of nickel to iron in cores from

the Pacific, as compared with that in the

earth's crust. Although the terrestrial

abundances agree best with those of the

deep-sea deposits, this does not necessarily

imply a terrestrial origin for the latter.

The earth's outer crust itself, being the last

addition to our planet from cosmic sources,

may be built of a material whose remnants

are still falling on the earth from the

zodiacal-light cloud.

1956. Interplanetary dust and terrestrial

accretion of meteoric matter. Irish

Astron. Journ., vol. 4, pp. 84-135.

In a long and detailed discussion the

author considers a number of processes

of accretion and evaluates limits for particle sizes and amounts. The radius for

metallic particles in interplanetary space

has a lower limit of 7.2 X 10~6 cm because of

radiation pressure. For compact stone

fragments the lower limit is 1.9X10"5 cm.

Zodiacal dust is the main source of terrestrial accretion, and direct collision is

the most important process. With a

space-density of zodiacal dust of 2X10~21

gm/cm3, the total accretion is most probably

0.051 grams in 106 years per horizontal

square centimeter of earth's surface, or

250,000 tons of meteoric dust per year over

the entire surface of the earth. A table is

included of the relative abundances of

nickel, cobalt, and copper.

OTT, J. (see under Linke and Ott)

OVENDEN, M. W.

1951. Meteors and space travel. Journ.

British Interplanetary Soc, vol. 10,

p. 176ff.

Present observations indicate a negligible danger to an interstellar rocket of

collision with interstellar dust particles.

PACKER, D. M., AND LOCK, C.

1950. The brightness and polarization of the

daylight sky at altitudes of 18,000

to 38,000 feet above sea level.

Naval Res. Lab. Report 3713,

July 31.

The data indicated the presence of large

scattering particles in the atmosphere above
102 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

the observers at all altitudes. Observations were made from a B-29 over Arizona,

over southern California, and over western

Canada, flying at 27,500 feet over snow

fields and at 3,400 feet over cloud layer.

PALMIERI, P.

1879. Studies of dust collected on February

25, 1879 in Portici. Rend. R. Ace.

Sci. Fis. Naples, vol. 18, p. 112ff.

(In Italian.)

The author found Fe3O4 by use of a

magnet, but did not find Fe or effervescence with acids.

1901. On terrestrial and cosmic dust, and

the African sands. Analysis and

discussion. Rend. R. Ace. Sci.

Fis. Naples, ser. 3, vol. 7, pp. 156,

163, 172. (In Italian.)

The author gives the history of the fall

of March 10, 1901, and states that particles

of Fe3O4 were found.

PATON, J.

1951. Auroras and luminous night clouds.

Nature, vol. 168, pp. 487-488.

The nature and origin of the clouds are

still uncertain. Meteoric dust would tend

to drift to and remain below the base of

the temperature inversion at 80 km. The

presence of the clouds at this level is in

itself evidence for the existence there of a

temperature minimum.

PENNISTON, J. B.

1931. Note on the origin of loess. Pop.

Astron., vol. 39, pp. 429-430.

The author proposes meteoric dust as the

origin.

1942. Detailed description of the zodiacal

light. Pop. Astron., vol. 50, pp.

547-552.

This paper, based largely on observations by G. Jones during Perry's expedition to Japan, 1853-1856, favors the theory

that zodiacal light is a ring or disc around

the sun.

PETTERSSON, H.

1949. Exploring the bed of the ocean.

Nature, vol. 164, pp. 468-470.

This general article mentions tiny meteoritic pellets as part of the deposit.

1955. Magnetic spherules and meteors.

Naturwiss., vol. 42, pp. 387-388.

(In German.)

The paper summarizes the results of

research on iron spherules collected by the

Swedish Deep-sea Expedition of 1947-

1948. The number of magnetic spherules

collected from Pacific Ocean sediments

(nearly 1,000 per kilogram of sediment) is

20 to 40 times greater than the number

previously found. The spherules occur to

a depth of at least 3 meters under the

sediment area, indicating a deposit age of

from 1.5 to 3 million years.

1960. Cosmic spherules and meteoritic dust.

Sci. American, vol. 202, no. 2,

pp. 123-132.

A plausible figure for the amount of

meteoritic dust landing on the earth is

5 million tons per year. The figure is

based on the author's measures of deep-sea

cores and of samples obtained in Hawaii,

and on values given by other scientists.

— AND ROTSCHI, H.

1950. Nickel-content of deep-sea deposits.

Nature, vol. 166, p. 308.

Preliminary results from the Swedish

Deep-Sea Expedition of the Oceanografiska

Inst., Goteborg. If the nickel found is of

meteoritic origin the apparent rate of

accretion is estimated at several thousand

tons a day, which is considerably more than

astronomers get on the basis of visual and

telescopic counts of meteors entering the

atmosphere.

1952. The nickel content of deep-sea deposits. Geochim. et Cosmochim.

Acta, vol. 2, pp. 81-90.

Determinations of the amounts of nickel,

manganese and iron present in sediment

cores from the central Pacific Ocean have

been made by microchemical methods.
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 103

The nickel content in most cores was much

higher than the average value for continental rocks and sediments, with maximum

values ten times higher than the continental average. The highest nickel values

were found in material with a low rate of

sedimentation (of the order of 1 millimeter

in 1,000 years).

The authors found considerable variation

with depth in the nickel content below the

sediment surface. No correlation with

manganese and iron contents was evident

except in places where a change in the rate

of sedimentation appears to have affected

all three elements similarly.

The authors tentatively suggest that the

abyssal nickel may derive partly from the

settling of cosmic dust over the earth's

surface.

PICH, R. (see under Schoenberg and Pich)

PIOTBOWSKI, S. L.

1952. The collisions of asteroids. Astron.

Journ., vol. 57, p. 23.

Several million tons of matter are pulverized to dust annually by collisions between minor planets. This dust is thought

to replenish the dust of the zodiacal light

that slowly spirals into the sun.

RAMAGE, H. (see under Hartley and Ramage)

RANYARD, A. C.

1878. On the presence of particles of iron in

the atmosphere. Astron. Register, vol. 16, pp. 299-300.

This paper, abstracted as read at the

meeting of the Royal Astronomical Society,

Nov. 8, 1878, discusses Murray's deep-sea

magnetic globules, Nordenskiold's snow

samples, Flight's experiments, and Ranyard's observations on shipboard.

1879. Note on the presence of meteoric

dust in the atmosphere. Monthly

Notices Roy. Astron. Soc. London,

vol. 39, pp. 161-167.

REDMAN, R. O.

1959. Dust and gas between the earth and

the sun. The Observatory, vol. 79,

pp. 172-181.

The distribution of gas and dust is fairly

continuous between the sun and the earth.

Blackwell's photography from aircraft at

eclipses, with subsequent measures and

analyses, has closed the gap between the

corona and the zodiacal light measures.

Evidence shows a variability of the zodiacal

light, which probably results from variation in the number of electrons in the gas

rather than from a changing amount of

dust. Although satellite research, with

measurements from places far beyond the

moon, will be valuable in later years, the

best optical techniques used either from

the ground or from conventional aircraft

can still add to our present knowledge.

REICHENBACH, K. L. F. VON

1859. Captain Callum's meteoric spherules.

[Poggendorf's] Annalen der Physik

und Chemie, ser. 2, vol. 106,

pp. 476-490. (In German.)

The author discusses meteoric dust from

the Joshua Bates, 1856, and argues against

Ehrenberg's volcanic theory to explain

these spherules. He concludes that the

Fe3O4 dust of a great iron or iron-rich

meteor had fallen upon the deck of the

Joshua Bates, and that the sample submitted to Ehrenberg showed what the train

of such a meteorite consists of.

RENARD, A. V. (see under Murray and Renard)

REVELLE, R. R.

1944. Marine bottom samples collected in

the Pacific Ocean by the Carnegie

on its seventh cruise. Carnegie

Inst. of Washington, Publication

No. 556, pp. 1-180.

One magnetic spherule was found in red

clay. The author quotes Murray on cosmic

constituents.
104 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

RlCHTER, N .

1955. Experimental investigations concerning the illumination of clouds of

reflecting particles. M6m. Soc.

Roy. Sci. Liege, ser. 4, vol. 15,

pp. 80-88.

The author investigated the illumination

of clouds of reflecting particles by experiments on small grains of various metals.

RINEHART, J. S. (see also under Hodge and

Rinehart)

1957a. Distribution of meteoritic debris

about the Arizona meteorite crater.

Smithsonian Contr. Astrophys., vol.

2, pp. 145-160.

The author systematically investigated

the distribution of meteoritic dust and of

bits and pieces of meteoritic material scattered in the soil around the Arizona

Meteorite Crater, in order to fix the direction of flight and the mass of the meteorite

that made the crater.

Seven hundred samples of soil were collected from an area of 80 square miles

around the crater. Three types of strongly

magnetic material were separated from the

soil: (1) particles of nickel-iron; (2) ironoxide particles; and (3) black shiny particles, probably bits of magnetite. The

author concludes that 12,000 tons of meteoritic material surround the crater in the form

of dust. He believes that the meteorite

approached from a southwest direction and,

when it hit the earth, pitched forward large

amounts of fragmented and molten

material.

1957b. A soil survey around the Barringer

Crater. Sky and Tel., vol. 16,

pp. 366-369.

The author gives a popular presentation

of the data given in Rinehart (1957a).

ROTSCHI, H. (see under Pettersson and Rotschi)

ROY, F. DE

1935. Report of Commission 22. Transactions of the Int. Astron. Union, vol.

5, pp. 326-328, 373-374.

It is important to determine if the magnetic metallic dust present in the atmosphere is of meteoric origin. This dust can

easily be collected by simple methods.

Simultaneous observations in different regions could eventually establish a correlation between the number of metallic

particles collected and periods of meteoric

activity. If a sufficient quantity could be

collected, it might be submitted to chemical

analysis.

1938. Item 9 on meteoric dust. Transactions of the Int. Astron. Union,

vol. 6, p. 160. (Abstract.)

The problem of the origin of metallic dust

deposited from the atmosphere or found in

the soil or on the ocean floor has recently

attracted renewed attention. From 10-day

collections of such dust made in July to

October during the years from 1927 to 1936,

L. Rudaux infers that magnetic particles

were more plentiful at the beginning of

August, and finds another maximum at the

end of August and in early September. In

1928 and 1933, copious deposits also occurred in October (Giacobinids). Systematic observations are desirable.

RUDAUX, L.

1930a. Meteors. L'Ulustration, vol. 88, p.

513ff. (In French.)

Magnetic dust-deposits are more abundant in the period of the year that is rich in

meteors. The number of such particles

does not increase proportionally with the

very variable deposits of atmospheric dust.

At Donville the deposits are even more

abundant when the wind blows constantly

off the sea. Two days after the passage

of a great bolide in September 1927, the

fragments were so voluminous that they

could be seen with the naked eye on the

receiving surface. The author thinks this

tends to break down the distinction between

meteors and bolides.

1930b. Meteors and the earth. Aerial dust.

La Nature, vol. 58, part 2, p. 439ff.

(In French.)

In this general, illustrated article, the

author discusses magnetic particles of

extraterrestrial origin.
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 105

1933. Magnetic particles collected after the

meteor shower of October 9. La

Nature, vol. 61, part 2, p. 436ff.

(In French.)

The author describes a meteor shower

followed by a dust shower.

SCHOENBERG, E.

1941. On the position of the axis of the zodiacal light. Astron. Nachr., vol 272,

p. 25ff. (In German.)

The author opposes Hoffmeister's views.

AND VAUCOULEURS, G. DE

1952. Meteorites. Manuel Pratique d'Astronomie, pp. 239-242. (In

French.)

Microscopic meteoritic particles or remains of their disintegration are continuously received by the atmosphere, as proved

by particles found abundantly on the snows

of high mountain summits or on polar

glaciers. Small particles were especially

numerous after the meteor shower of October 9, 1933.

SANDIG, H.

1941. The spatial arrangement of the zodiacal light material. Astron. Nachr.,

vol. 272, p. 1.

The author does not support Hoffmeister's theory.

SCHEWICK, H . VAN

1939. Mass and density of the zodiacal light.

Vierteljahrschrift Astron. Gesellschaft, vol. 74, p. 233ff. (In

German.)

SCHLOSS, L.

1935. Meteoric dust. Pop. Astron., vol.

43, pp. 63-64.

The author describes a first attempt at

collecting meteoritic dust by means of a

magnet.

SCHMID, F.

1928. The zodiacal light, its nature and its

cosmic or terrestrial formation.

Hamburg, 128 pp. (In German.)

1940. New contributions to the problem of

the zodiacal light. Astron. Nachr.,

vol. 270, p. 220ff. (In German.)

Some inconsistencies might be explained

if the zodiacal light were considered as part

of the earth's atmosphere.

AND PICH, R.

1939. Investigations of the zodiacal light.

Mitt. Univ. Sternwarte Breslau,

vol. 5, p. Iff. (In German.)

This paper presents a study based on

observations made in the tropics, and includes a section on the height of the earth's

atmosphere at which light scattering occurs.

SCHUSTER, A.

1882. B.A.A.S. report of the committee on

meteoric dust. Nature, vol. 26, p.

488. (Abstract.)

All the volcanic dust that the author had

at his disposal was carefully examined

under the microscope, and its appearance

found to be altogether different from the

supposed meteoric dust. The author

agrees with Tissandier.

SEARLE, A.

1899. The zodiacal light. Astrophys.

Journ., vol. 8, pp. 244-245.

Progress of knowledge of the subject

removes the difficulties attending the

hypothesis that the zodiacal light is bight

reflected from meteoritic dust forming a

part of the solar system. Lambert's

theory is found inapplicable.

SEATON, M. J. (see under Kaiser and Seaton)

SEELY, B. K. (see under Crozier and Seely)

SEN GUPTA, P. K.

1954. Periodic influx of interplanetary dust

particles into the terrestrial atmosphere. Indian Journ. Meteorol. Geophys., vol. 5, pp. 272-276.

The author gives a brief review of earlier

papers relating to the influx of interplanetary dust particles to the terrestrial

atmosphere. He favors the theory that
106 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

solar corpuscular streams repeatedly push

the particles towards the earth and concentrate them near the earth and in the

ecliptic.

SIEDENTOPF, H. (see under Behr and Siedentopf)

SLIPHEB, V. M.

1931. A preliminary note on the spectrum

of the zodiacal light. Lowell Observatory Circular, February 20.

The author obtained spectra with dispersion 6 mm from H to K. Keflected sunlight with superposed emissions suggests

that the zodiacal light arises in part in the

earth's atmosphere.

SLOCUM, F.

1934. Iridescent clouds and cosmic dust.

Journ. Roy. Astron. Soc. Canada,

vol. 28, pp. 145-148.

SHALES, A. A.; MAPPER, D.; AND WOOD, A. J.

1958. Radioactivation analysis of "cosmic"

and other magnetic spherules.

Geochim. et Cosmochim. Acta, vol.

13, pp. 123-126.

By neutron activation analysis, the

authors found the chemical content of

magnetic spherules to lie in the range 0.03

to 3.9 micrograms for nickel, 0.01 to 0.3

micrograms for cobalt, and 0.0006 to 0.53

micrograms for copper. From the ratios

of nickel to copper, nickel to cobalt, copper

to cobalt, and nickel to iron, two samples

from deep-sea cores are identified as being

closely related to iron meteorites. A sample from the roof of a station off the coast

of Sweden and another from sand of the

River Danube have quite different chemical compositions.

AND WISEMAN, J. D.

1955. Origin of nickel in deep-sea sediments.

Nature, vol. 175, pp. 464-465.

The ratios of nickel to cobalt, nickel to

copper, and copper to cobalt are 13.1, 92,

and 0.14 for meteorites, and 3.5, 1.1, and

3.0 for igneous rocks. Using radioactivation methods on samples of globigerina

ooze, red clay, and oceanic rocks from the

Atlantic, Pacific, and Indian Oceans, the

authors found that meteoritic material

made little significant contribution to deepsea sediments, unless some remarkable

differential behavior of the three elements,

nickel, cobalt, and copper, has taken place.

SPENCER, L. J.

1933. Meteoric iron and silica glass from the

meteorite craters of Henbury (Central Australia) and Wabar (Arabia).

Mineralog. Mag., vol. 23, pp. 387-

404.

Spherical particles resembling meteoritic

dust were found.

STAUDE, N.

1923. On the astronomical theory of meteors. Astron. Nachr., vol. 218, p.

155ff. (In German.)

The author discusses the daily variation

in the brightness of the night sky on the

basis of the meteoritic hypothesis for the

zodiacal light. There are comments by C.

Hoffmeister.

STOIBER, R. E.; LYONS, J. B.; ELBERTY, W. T.;

AND MCCREHAN, R. H.

1956. The source area and age of Ice-Island

T-3. Final Report under Contract AF19(6O4)-1O75, Dartmouth

College, Department of Geology.

The authors identified magnetic spherules found in deep cores in Arctic IceIsland T-3 as probably extraterrestrial.

The composition was magnetite and the

surfaces were sometimes striated. Particle

size ranged from 5 to 100M and more.

STRUVE, O.

1943. Recent progress in astrophysics: V. G.

Fesenkov's dynamical theory of

the zodiacal light. Astrophys.

Journ., vol. 98, pp. 129-130.

1951a. Dust in the solar system. Sky and

Telescope, vol. 10, pp. 88-91.

The author gives a general review of

relevant current literature.
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 107

1951b. Photography of the counterglow.

Sky and Telescope, vol. 10, pp.

215-218.

In addition to describing the wide angle

equipment constructed by Greenstein and

Henyey, Struve reviews the theory by

Fesenkov that the gegenschein or "false

zodiacal light" is the earth's tail. He also

presents the arguments of M. G. Karimov

and of N. B. Divari opposing this view.

SVESTKA, Z.

1950. A note on the brightness of lunar

eclipses. Bull. Astron. Inst. Czechoslovakia, vol. 2, pp. 41-43.

The author discusses the variation of the

brightness of lunar eclipses with respect to

an atmospheric dust layer. An earlier

theory of a yearly periodicity is replaced

by the theory that the brightness may

depend in part on the quantity of meteoric

dust in the earth's atmosphere.

1954. The problem of a meteoritic dust

layer in the earth's atmosphere.

Bull. Astron. Inst. Czechoslovakia,

vol. 5, pp. 91-98.

The author discusses again the evidence

for a high atmosphere dust layer, as

deduced from lunar eclipse observations.

He calculates that only particles of radius

10~5 or 10~8 cm are consistent with the

observations. Such small particles would

have to be carried to the lower parts of the

atmosphere much faster than the rate

computed for a quiet atmosphere. The

author believes that turbulence could do

this.

SWINGS, P.

1949. The spectra of the night sky and the

aurora. In, Kuiper, ed., The atmospheres of the earth and planets,

pp. 159-212.

THERNOE, K.

1941. The zodiacal light. Nordisk Astron.

Tidsskrift, vol. 22, pp. 73-80. (In

Danish.)

The author discusses various problems

of the zodiacal light.

THIESSEN, G.

1948. Associations between the solar corona

and the zodiacal light. Himmelswelt, vol. 55, p. 161ff. (In German.)

The interplanetary dust-cloud is discussed.

THOMSEN, W. J.

1953. The annual deposit of meteoritic dust.

Sky and Telescope, vol. 12, pp.

147-148.

The author collected magnetic spherules

from rooftops and buckets in Iowa City.

He assumed that they were meteoritic.

Spectroscopic analysis of the magnetic

spheres showed iron, silicon, and magnesium. A gravimetric check gave SiO2,

28 percent; Fe2O3, 72 percent. No nickel

was detected. The spheres were 8 to 80/x

in diameter. The rate of fall was calculated to be 2 X 109

 kg/yr for the entire

earth.

TISSANDIEB, G. (see also under Meunier and

Tissandier)

1875. On the existence of iron and magnetic

particles in atmospheric dust.

Comptes Rendus, Paris, vol. 81,

p. 576ff. (In French.)

The author concludes that some magnetic particles are not terrestrial in origin.

TROWBRIDGE, C. C.

1907. Physical nature of meteor trains.

Astrophys. Journ., vol. 26, pp. 95-

116.

Meteor trains are self-luminous gas

clouds combined with very minute meteoric dust particles; the latter in daylight

reflect light like ordinary clouds.

TSCHERKASS, W. K. (see under Tscherwinsky

and Tscherkass)

TSCHERWINSKY, P. N., AND TSCHERKASS, W. K.

1929. On why it is so difficult to prove the

presence of cosmic dust on the surface of the earth. Mirov6d6ni6,

vol. 18, No. 2; Centralblatt Min.

Geol. Pol., Abt. A, pp. 127-129.
108 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

The authors compute that only 0.00007

milligram of meteoritic dust falls per square

meter, annually.

VAETH, J. F.

1951. 200 miles up (the conquest of the

upper air). New York, 207 pp.

The author discusses atmospheric dust

on pages 24-25 and 67.

VAUCOULEURS, G. DE (see under Rudaux and de

Vaucouleurs)

VEGARD, L.

1923a. The constitution of the upper strata

of the atmosphere. Philos. Mag.,

vol. 46, p. 557ff.

The author assumes a dust atmosphere

above the gaseous atmosphere, the gaseous

ending at about 80-100 km above the

surface, with the dust comparatively dense

at 100-120 km, slowly decreasing upward.

1923b. Distribution of matter in the highest

strata of the atmosphere. Videnskapsselskapets Skrifter, Mat.-

Naturv. Klasse (Kristiania), no.

10.

The author discusses nitrogen dust in

the upper atmosphere, the tendency for

electrified dust to drift toward the magnetic equator, and the bearing of his

theory on the interpretation of the zodiacal

light and gegenschein.

1923c. On the constitution of the upper layers

of the atmosphere. Comptes Rendus, Paris, vol. 176, p. 1488ff. (In

French.)

This paper discusses nitrogen dust in the

highest layers of the atmosphere, and its

bearing on color changes along the paths

of meteors.

VOLZ, F., AND GOODY, R. M.

1960. Twilight intensity at 20° elevation.

Scientific Report No. 1, pp. 1-46,

on Air Force Contract AF19-

604(4546), Blue Hill Meteorological

Observatory, AFCRC-TN-60-284,

1960.

The authors designed a photometer to

measure the absolute intensity of the twilight in five narrow bands of wavelengths

from the red to the ultra-violet region of

the spectrum. Gradients of the logarithm

of intensity and color ratios give complex

but sensitive indicators of dust scattering,

which is small but measurable if precise

absolute methods are used. The problem

is very complex, but the authors think that

useful information can be obtained up to

120 km for observations in blue light, and

up to 75 km for observations in red light.

WATSON, F. G.

1956. Between the planets. Ed. 2, Cambridge.

WEIL, M.

1922. Theories on the nature of meteor

trains, with a note on Professor

Trowbridge's contributions to our

knowledge of meteor trains. Pop.

Astron., vol. 30, pp. 524-535.

The paper gives a historical bibliography,

including references to reflection and other

theories that assume meteor trains are composed of cosmic dust or a disintegrated

meteoroid.

WHIPPLE, F. J. W.

1934. Phenomena related to the great Siberian meteor. Journ. Roy. Meteorol. Soc, vol. 60, pp. 505-513.

Concerning the illumination of the sky

on the nights following the arrival of the

meteor, the author suggests that the meteor

had a tail that was captured by the earth's

atmosphere.

WHIPPLE, F. L.

1949. Report of Commission 22. Transactions of the Int. Astron. Union, vol.

7, pp. 240-244.

Meteoritic dust has been collected by

H. H. Nininger and H. E. Landsberg, and

its consequences considered theoretically

by J. Kaplan and A. R. Khan.

1951a. Comets and the zodiacal light.

Astron. Journ., vol. 56, p. 51.

(Abstract.)

The icy-conglomerate model of comets,

coupled with the Poynting-Robertson effect
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 109

and planetary perturbations, provides the

required rate of addition of material to

the zodiacal cloud and also predicts the

required distribution of particle sizes.

1951b. Origin of the zodiacal light. Sky and

Tel., vol. 10, p. 94.

The author suggests that particles are

blown off comets when icy surfaces of the

comets vaporize in sunlight; the particles

then spiral around the sun to form the zodiacal light.

1952a. Report of Commission 22. Trans. Int.

Astron. Union, vol. 8, pp. 293-300.

Work in Czechoslovakia included investigation by M. Plavek on the PoyntingRobertson effect, the age of showers, and

the dimensions of comets; Link studied

the concentration of meteoritic dust falling

through the atmosphere. In Japan, Huruhata carried out investigations on the light

of the night sky and the zodiacal light;

he found a relation between the zodiacal

light and Comet Encke, and between the

zodiacal light and the solar corona. In

the U.S.S.R., Fesenkov's work on meteoritic matter in interplanetary space dealt

also with the zodiacal light. Astapovich

and Khvostikov studied noctilucent clouds

and found that they are not caused by

meteoritic dust but by condensation of

water vapor.

1952b. Results of rocket and meteor research.

Bull. Amer. Meteorol. Soc, vol. 33,

pp. 13-25.

This paper discusses the pitting of shiny

surfaces of rockets probably by micrometeorites, and the possibility of their contributing to E-layer ionization, light scattering, and twilight sodium radiation.

1955a. A comet model. III. The zodiacal

light. Astrophys. Journ., vol. 121,

pp. 750-770.

The author considers the probable cometary contributions to the zodiacal cloud

on the basis of the icy-comet model. He

assumes the zodiacal cloud to be of the

nature deduced by van de Hulst and Allen

from their studies of the Fraunhofer

corona and the zodiacal light. According

to the Poynting-Robertson effect, the

zodiacal cloud needs for its maintenance

about 1 ton/sec of small particles in the

10~4 to 1.0 cm range. Comets continuously contribute some 30 tons/sec. They

lose matter by the following four physical

forces or processes: (1) interstellar wind,

(2) Jupiter's random perturbations, (3) the

Jupiter perturbation barrier, and (4) collisional destruction. The first and fourth

of these seem to be the most important.

Collisions among the particles seem to be

most responsible for the cutoff in zodiacal

particle size above 0.03 cm, as found by

van de Hulst.

If it is great enough, corpuscular radiation may be more important than the

Poynting-Robertson effect; it may also require more material for the zodiacal cloud.

If this is true, corpuscular radiation will

increase the critical cutoff dimension.

1955b. On the origin of the zodiacal particles.

Me'm. Soc. Roy. Sci. Ltege, ser. 4,

vol. 15, pp. 183-184.

The author states that the PoyntingRobertson effect requires approximately

one ton/sec of small particles 10~4 to 1.0 cm

in diameter to maintain the zodiacal cloud.

Consideration of the effect of corpuscular

radiation may indicate a considerably

larger source of material for the zodiacal

cloud. The probable contribution to the

zodiacal cloud from comets is considered

on the basis of the icy comet model.

1958. The meteoric risk to space vehicles.

Proc. 8th Int. Astronaut. Congr.

Barcelona, 1957, pp. 418-428.

The author discusses the distribution and

rate of fall of meteoritic material as functions of mass and velocity, and presents

a table concerning meteoroids and gives

formulas for computing the probabilities of

penetration in space vehicles. The author

calculates upper limits for the effects of

erosion on a space-exposed surface subject

to erosion by meteoritic dust, corpuscular

radiation from the sun, and gases of the

extended solar corona. He concludes that
110 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

the corrosive effect from meteoritic dust is

comparable to the combined effects from

the other two factors.

1959. Solid particles in the solar system.

Journ. Geophys. Res., vol. 64,

pp. 1653-1664.

The author discusses the present state

of our knowledge concerning solid particles

in the solar system. Our best information

comes primarily from studies of optical

meteors, radio meteors, the zodiacal cloud

and meteorite analysis. Both space observations and ground-based experiments are

important for the future. The author

believes that 70 to 90 percent of the

expected results from meteoritic studies can

be provided from the ground, but such

observations cannot give good information

on solid particles in space much beyond

1 a.u., and unexpected results may come

from space observations.

Detailed knowledge of particles in the

solar system is of practical importance to

designers of space equipment and to

operational planners. Theoretically, meteoritic material can provide basic information on the evolution of the earth and the

solar system. He discusses possibilities for

meteorite instrumentation in space vehicles.

AND GOSSNER, J. L.

1949. An upper limit to the electron density

near the earth's orbit. Astrophys.

Journ., vol. 109, pp. 380-390.

Brightness and polarization observations

are used. Observed polarization can probably be accounted for by the reflection of

sunlight by dust particles.

—AND HAWKINS, G. S.

1956. On meteors and rainfall. Journ. Meteorol., vol. 13, pp. 236-240.

The authors consider the role of micrometeorites that enter the atmosphere without producing detectable light or ionization.

A large number of micrometeorites in a

stream could affect rainfall. To explain

the removal of particles from the stream

the authors suggest a mechanism that

depends upon the gradual disintegration

of micrometeorites under the influence of

corpuscular radiation from the sun. The

rate of orbital spiralling is calculated to

be 15 times greater than that due to the

light pressure component of the PoyntingRobertson effect. To affect amounts of

rainfall, more cometary material than was

originally postulated to supply the zodiacal

cloud would be necessary.

WILDT, R. (see under Hodge and Wildt)

WISEMAN, J. D. (see under Smales and Wiseman)

WOOD, A. J. (see under Smales, Mapper, and

Wood)

YAGODA, H.

1959. Observations on nickel-bearing cosmic

dust collected in the stratosphere.

Geophysics Research Directorate

Research Notes No. 9, AFCRCTN-59-200, ASTIA Document No.

AD-212422, pp. 1-13.

The author used microchemical methods

to examine stratospheric dust particles

collected on four balloon flights at altitudes

between 77,000 and 112,000 feet. Collections were made on simple plastic dishes

mounted at the top of the balloon and at

the gondola level, with continuous exposure at both levels. The preliminary

data showed that the relative abundance

of nickel-bearing dust ranged between 0.17

and 0.36 particle per cm2 of collection

surface per day of exposure. Most of the

color reactions for nickel were given by

particles of diameters between 20 and 40M,

but positive reactions were also given by

smaller particles with diameters of 1 to 2ju.

YAMAMOTO, I.

1938. Report of the sub-commission on

zodiacal light. Trans. Int. Astron.

Union, vol. 6, pp. 172-175.

The author summarizes theories on the

nature of the zodiacal light by Hoffmeister,

Schmid, Brunner, Larmor, and Donitch,

and brings out the major differences in

these theories.
ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 111

YAVNEL, A. A.

1957. Meteoritic matter at the place of fall

of the Tunguska Meteorite. Russian Astron. Journ., vol. 34, pp.

794-796. (In Russian.) English

translation by F. W. Wright and

P. W. Hodge, Tech. Rep. No. 7,

AF18(6OO)-1596, ASTIA Document No. AD 154 146, 1958.

The author gives results of investigations of the magnetic portion of soil

samples collected in 1927 to 1930 at the

place of fall of the Tunguska meteorite.

Visual examination with a microscope

showed small metallic particles and black

shiny globules of magnetite, 30 to 60/x in

diameter. Spectroscopic analysis showed

that the particles are composed of nickeliron. The author concludes that these

particles are part of the Tunguska meteorite, which was evidently an iron. The

data show a great similarity with those for

the Sikhote-Alin meteorite, as determined

by Krinov and Fonton (1952, 1954).

YoKOYAMA, E.

1950. Interim report on observations of atmospherics which may be caused

by meteoric showers. Proc. Imp.

Acad. Tokyo, vol. 6, p. 154ff.

YUDIN, I. A. (see under Kolomensky and

Yudin).

YUNG, E.

1883. A fall of cosmic dust. Comptes Rendus, Paris, vol. 97, p. 1449ff. (In

French.)

The paper describes the great snowfall

of Wednesday, December 5, 1883, at

Geneva. The author notes that fine metallic dust is prevalent after the times of

meteor showers and believes the dust is due

to the rupture of a large meteorite and to

microscopic meteorites.

ZACHAROV, I.

1952. Influence of the Perseids on atmospheric transparency. Bull. Astron.

Inst. Czechoslovakia, vol. 3, pp.

82-85. (In French.)

Measures of the darkness and size of the

earth's shadow during lunar eclipses show

that after the appearance of several of the

most active meteor streams, our atmosphere is polluted in the upper region by

dust. These are either interplanetary dust

particles or the residue of meteors, which

dissipate at 80 to 150 km. The author

uses limited Mt. Wilson measurements to

show that a slight decrease in the amount

of atmospheric transparency follows a meteor shower. The relatively short duration

of the depression is inconsistent with the

time of fall of the particles. This discrepancy is explained by the agglomeration of

particles, which diminishes their absorbing

power and increases the speed of fall. The

pollution of the atmosphere has a maximum duration of 24 days. Particles with

diameters less than 0.1/u and of density 4

would fall for some tens of years.

ZIMMERMANN, H. (see under Hoppe and Zimmermann)