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

This series, Smithsonian Contributions to Astrophysics, was inaugurated in 1956 to provide a proper communication for the results of research con- ducted at the Astrophysical Observatory of the Smithsonian Institution. Its purpose is the "increase and diffusion of knowledge" in the field of astrophysics, with particular emphasis on problems of the sun, the earth and the solar system. Its pages are open to a limited number of papers by other investigators with whom we have common interests. Another series is Annals of the Astrophysical Observatory. It was started in 1900 by the Observatory's first director, Samuel P. Langley, and has been published about every 10 years since that date. These quarto volumes, some of which are still available, record the history of the Observatory's researches and activities. Many technical papers and volumes emanating from the Astrophysical Observatory have appeared in the Smithsonian Miscellaneous Collections. Among these are Smithsonian Physical Tables, Smithsonian Meteorological Tables, and World Weather Records. Additional information concerning these publications may be secured from the Editorial and Publications Division, Smithsonian Institution, Wash- ington, D.C. FBED L. WHIPPLE, Director, Astrophysical Observatory, Cambridge, Mass. Smithsonian Institution.

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 AHNERT, E. compilation of references to significant papers 1954. Preliminary report on attempts to de- relating to the study of interplanetary dust. tect meteoritic dust. Die Sterne, Some references have been included from vol. 30, pp. 36-38. (In German.) Bibliography on Meteoritic Dust with Brief The lack of nickel in the spherules col- Abstracts compiled by Hoffleit (Harvard College lected by Thomsen (1953) casts doubt on Observatory Reprint Series n-43, 45 pp., 1952), their interplanetary origin. Hoffmeister and now out of print. has collected dust in the neighborhood of In the selection of references from the factories and has found spherules (45 to Hoffleit bibliography, we have attempted to 135jt in diameter) similar, at first glance, to include all important papers as well as repre- Thomsen's spherules, but nonmagnetic. sentative samples that are of special interest Collections from more isolated regions con- for historical reasons. tained no spherules. Collections from snow In the selection of references published since showed no spherules but did show irregular the appearance of the Hoffleit bibliography, we particles, 15 percent of which were mag- have been guided by the main principles that netic, with diameters of 100 to 200M- Hoffleit adopted for her compilation: Three types of dust have been considered as meteor- ALLEN, C. W. itic dust in the search for material: particles that enter 1956. Influence of solar atomic emission on the upper atmosphere as minute dust particles (the the orbits of interplanetary parti- zodiacal light may be a source of such); dust products cles. Observatory, vol. 76, pp. of the disintegration of larger meteoroidal masses during their passage through the atmosphere; and 101-103. possible pulverized remnants of meteorite-impacts. The author discusses the magnitude of In addition, we include some papers relating the collision effect and shows that the rate to interplanetary dust outside the earth's at which particles approach the sun may be atmosphere. greater than that indicated by calculations As far as practicable, the titles of journals based on the Poynting-Robertson effect. appear in the original language of publication. He does not consider the influence of large- For maximum usefulness to the reader, how- scale solar magnetic fields. ever, titles of papers are given in English. ANGSTRSM, A. Papers written in a language other than 1929. On the atmospheric transmission of English are usually indicated by a parenthetical sun radiation and on dust in the note. air. Geografiska Annaler, vol. 11, p. 156ff. 1 Harvard College Observatory and Smithsonian Astropbyslcal Ob* servatory, Cambridge, Mass. The author studies the effect of dust on •Maria Mitchell Observatory, Nantuckct, Mass., and Yale Uni- versity Observatory, New Haven, Conn. measurements of the solar constant; he be- 86 86 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS lieves that dust of cosmic origin may be lists of bolides observed in the U.S.S.R. characterized by particles of smaller size Chapters 34 and 35 deal with meteoric than those of volcanic origin or of dust and cosmic dust in the earth's atmosphere, brought by convection from the earth to and meteoric material on the earth's the atmosphere. surface. The author gives a review of work done by others on meteoric and cosmic ANONYMOUS dust in the earth's atmosphere and on 1885. Meteoric dust. Sci. American, vol. meteoric material on the earth's surface. 52, p. 83ff. He concludes that more than 16,000 tons of The complete article reads: "A metallic meteoric material fall on the earth each substance in powder or small granules has year. been sent to the Science News laboratory for examination. It proves to be meteoric BARBIER, D. dust, largely composed of iron, nickel, and 1955. Variations in intensity of the zodiacal silica. Dr. Batchelder, of Pelham, N.H., light. M6m. Soc. Roy. Sci. Li6ge, who sent the specimen, states that he col- ser. 4., vol. 15, pp. 55-71. (In lected the dust on the walk in front of his French.) house after a smart thunder shower. It is The author describes his photoelectric probable that large quantities of this ma- measurements in three colors of the in- terial fall upon the earth, but remain un- tensity of the zodiacal light, and discusses noticed. Much of the iron found in soils is the variations of intensity and color with due to precipitation from interstellar time. spaces, the particles becoming entangled in our atmosphere." BARRINGER, D. B. 1909. Meteor crater in Northern Central ANYZESKI, V. Arizona. Pamphlet, National 1947. A conjecture on the nature of some Academy of Sciences, 24 pp. meteoritic matter. Pop. Astron., The author discusses small specks of vol. 55, pp. 169-171. meteoritic material admixed with rock The author suggests that some meteors fragments. may be solid hydrogen or ice with inclusions of ordinary meteoritic material. Some BEACH, A. bolides on entering the atmosphere may 1942. The zodiacal light. Astron. Soc. have a thick coating of hydrogen that Pacific, Leaflet No. 155, 8 pp. might account for some trains and might This is a historical note in popular style. explain the "nebulous meteors." BEARD, D. B. ARAGO, D. F. J. 1959. Interplanetary dust distribution. 1857. A list of the principal recorded show- Astrophys. Journ., vol. 129, pp. ers of cosmic dust. Astron. Popu- 496-506. laire, vol. 4, p. 208ff. The author maintains that the most reliable estimates of the concentration of ASTAPOVICH, I. S. of interplanetary dust depend upon our 1958. Bolides and their dust trains. In interpretations of measurements of Meteoric phenomena in the earth's scattered light observed in the solar corona atmosphere. State Publishing and in the night sky. On this basis, and House of Phys.-Math. literature, also from a theoretical discussion, he con- Moscow. (In Russian.) cludes that interplanetary dust is probably In Chapter 29 the author discusses distributed as r~3/a, where r is the distance bolides and their dust trains, and gives from the sun, and certainly the variation ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 87 of the dust concentration with solar 1953b. The structure of the zodiacal light. distance has this rate as an upper limit. Experimentia, vol. 9, pp. 134-135. He gives a few microns as the minimum (In German.) radius of the dust particles, and deduces At the Jungfraujoch the authors made that near the minimum particle radius, 3 8 photoelectric observations of the intensity the particle number varies as a" - , where and polarization of the zodiacal light. Chi a is the particle radius. The mass of all the the assumption that the polarization arises planets causes the dust to move towards from free electrons, the authors calculate a the ecliptic, and the distance from the space density of dust particles of 10~w/cm8, ecliptic is proportional to the solar distance which is nearly constant through the of the dust. The dust concentration at ecliptic. the earth's orbit is approximately 10~M to 15 3 10~ particles per cm , but at the earth's BOWEN, E. G. surface it is 10~10 to 10~" particles per cm3. 1953. The influence of meteoric dust on rainfall. Australian Journ. Phys., BEHR, A., and SIBDENTOPF, H. vol. 6, pp. 490-197. 1953a. Investigations of the zodiacal light Data on worldwide rainfall suggest a and the gegenschein from photo- correlation between rainfall and meteor electric measures on the Jungfrau- showers. In some localities heavy rainfalls joch. Zeitschr. Astrophys., vol. 32, tend to occur on certain days in a pattern pp. 19-50. (In German.) repeated yearly. The author suggests that The authors observed the brightness and meteoritic dust provides rain-forming nu- the polarization of the evening zodiacal clei when it enters cloud systems in the lower light by using a photoelectric photometer atmosphere. Particles with diameters of in two colors. They also observed the night 1 to 4/x require 30 to 50 days to fall to about sky in the region of the gegenschein. They 45,000 feet above the earth. This rate of interpreted the observations on the work- fall explains the 30-day lag between the ing hypothesis that the zodiacal light occurrence of the Geminid, Ursid, and material consists partly of free electrons, Quadrantid meteor showers, and the re- which cause the observed polarization, and corded maximum rainfalls. It is suggested partly of dust particles with radii greater that noctilucent clouds originate from than 10"* cm, which cause no noticeable meteoritic dust. polarization. For the space density of the electrons near the earth the authors give BRACEWELL, R. N. the value 600/cm3. The density rises in 1953. Meteors and rain. Observatory, vol. the ecliptic to around 1000/cm3 at 0.6 a.u. 73, pp. 249-250. from the sun, and falls to about 120/cm3 The author reports Bowen's findings on at 1.3 a.u. from the sun. The space density meteors and rainfall. of dust particles in the ecliptic outside Venus' orbit is constant, but inside Venus' BRIER, G. W. (see under Kline and Brier) orbit falls off somewhat towards the sun. The gegenschein has a simple explanation BULLRICH, K. if we accept the hypothesis that a cloud of 1949. Scattering of light on vapor and ice particles exists in the neighborhood of the particles. Zeitschr. f. Met., vol. libration point of the sun-earth system. 3, p. 335ff. (In German.) Here the particle density exceeds by 10 or The author discusses Link's attempt to 102 the general particle density in the determine the extinction coefficient of the ecliptic. air from measurements of light intensity at 88 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

the zenith. One difficulty is the uncer- COSARI, D. L. tainty of the scattering function, which 1834. Account of some remarkable hail- varies with the composition of aerosols in stones which fell at Padua on the the atmosphere. The theoretical scatter 26th of August, 1834. Ann. delle functions for water, dust, and ice, and for Scienze del Regno Lomb. Veneto various angles, are set up and compared (in Italian). See also Edinburgh with various experimental determinations. New Philosophical Journ., vol. 19, p. 83ff. (in English). BURGER, J. Among the large and very numerous 1949. Problems of cosmical aerodynamics. hailstones found, a great number con- Proceedings of symposium on the tained sandy matter. The author him- motion of gaseous masses of cos- self obtained only two such. In one there mical dimensions, Int. Union The- was only a minute quantity at the center. oretical and Applied Mechanics and In the other, the nucleus of ash-grey color Int. Astron. Union, edited by J. was about % inch in diameter and sur- Burger, 237 pp. rounded by pure ice. The minute amount While meteoritic dust as such is not dis- of dust gained from this sample was in- cussed, several of the papers on interstellar sufficient for chemical analysis. Some of matter have theoretical bearing, especially the grains were easily attracted by a papers by Spitzer, van de Hulst, and von magnet. It seemed probable that the dust Weissacker. was a combination of iron or nickel with some other unidentified substance. CHLADNI, E. F. F. CROZIER, W. D. 1819. On fireballs and dust-falls. Vienna, 1956. Rate of deposit in New Mexico of 434 pp. (In German.) magnetic spherules from the atmos- Chapter 6 contains reports in chronologi- phere (Abstract). Bull. Amer. cal order of falls of dust or fine material Meteorol. Soc, vol. 37, p. 308. in dry or moist form. Also, pages 20-23 This paper gives a condensed report of give a chronological table of supposed the collections of magnetic spherules found meteoritic dust-falls between the years 472 in New Mexico. The rate of deposit varies and 1816. Most of these are described as only slowly, and may be correlated with falls of red rain, red snow, or dust falls. meteor showers. There are no rapid More than 50 examples are given. changes in the rate of deposit which might be correlated with short-period meteor- CIALDEA, R. ological effects. 1950. The spectral distribution of polari- zation in skylight. Ann. Geofis., AND SEELY, B. K. vol. 3, pp. 357-370. (In Italian.) 1949. Some techniques for sampling and identifying participate matter in From observations of the degree of polar- the air. Technical Report No. ization of light from the sky, three typical 3-NR, Research and Development conditions are indicated in which the polar- Division, New Mexico School of ization increases, remains constant, or Mines, Socorro; Proceedings of the decreases with wave length. Theory shows First National Air Pollution Sym- that this relationship depends upon the posium, Pasadena. Abstracts: Pop. ratio of scatter from particles of molecular Astron., vol. 57, p. 459, 1949; Sky size to diffuse scatter from layers of large and Tel., vol. 9, p. 54, 1950. particles, the thickness of these layers Means have been developed for collec- determining the type of spectral distribution. tion of air-borne particles of sizes down to ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 89 well below one micron. Methods are given The author discusses the great flame ex- for combined microscopic and chemical plosion near Baku, Feb. 7, 1839, and a fall analysis. As a by-product of studies of of black, polished, hollow kernels similar to mass movements in the atmosphere, cosmic atmospheric iron dust found at the sea- dust in the air is being investigated. If bottom of the Pacific. tests show iron, nickel, and cobalt, the dust particles are probably of meteoric origin. ELBERTY, W. T. (see under Stoiber, Lyons, Elberty, and McCrehan). DAUBREE, A. 1893. Deep-sea deposits. Smithsonian an- FESENKOV, V. G. nual report for year ending June 30, 1938a. On the origin of the zodiacal light. 1893, p. 545ff. Comptes Rendus, Moscow, new The paper includes a section on mineral sef., vol. 19, p. 677ff. (In French.) substances of extraterrestrial origin (pp. 1938b. On the role of galactic matter in the 557-560), gives general discussion on the phenomenon of the zodiacal light. plausibility of finding meteoritic dust on Comptes Rendus, Moscow, new the sea-'bottom, and cites examples of ser., vol. 19, p. 451ff. (In French.) meteoritic dust accretion. In regard to the friable chondritic meteorites that fell at 1938c. Some considerations of the origin of Orgueil on May 14, 1864, the author com- the zodiacal light. Russian Astron. ments that if, instead of perfectly clear Journ.,vol. 15, p. 368ff. (In French.) weather, it had been rainy or the sky had 1940. The problems of the zodiacal light. been only covered with clouds through Russian Astron. Journ., vol. 17, p. which the stones would have had to pass, 25ff. (In Russian.) nothing could have been gathered up but a 1941. Investigation of the zodiacal light viscous mud. based on observations in the tropics. Russian Astron. Journ., vol. 18, p. DAVIDSON, D. T. (see under Handy and David- 3Iff. (In Russian.) son). 1942a. The dynamic theory of the zodiacal light. Russian Astron. Journ., vol. DURST, C. S. 19, pp. 28-49. (In Russian.) 1935. Dust in the atmosphere. Journ. Roy. 1942b. Minor planets and cosmic dust. Meteorol. Soc, vol. 61, pp. 81-87; Discovery, vol. 16, pp. 87-88. Doklady Acad. Sci. Report, vol. 34, pp. 163-167. (In Russian.) The paper gives a theoretical picture of a 1943. On the origin of the zodiacal light. dusty atmosphere in which each particle of dust is surrounded by a pocket of air having Doklady Acad. Sci. Report, vol. 39. temperature and humidity different from p. 377ff. (In Russian.) that of the general air mass. This picture 1945. Cosmic material and the zodiacal is corroborated by the rising of haze tops, light. Meteoritika, vol. 2, p. 3ff. the air temperature above the Arabian Sea (In Russian.) during the S.W. monsoon, and the diurnal 1946. On the motion of meteoric dust in variation of wind in that region. Some con- interplanetary space. Russian As- sequences are pointed out; one is that there tron. Journ., vol. 23, pp> 353-366. may be a layer of dust high up in the (In Russian with English abstract.) atmosphere. The author discusses the influence of gravity and radiation pressure. EHRENBERG, C. G. 1947. On the stability of the material of the 1858. Meteoric dust from the Joshua Bates. zodiacal light. Russian Astron. Monatsber. K. Akad. Wiss. Berlin, Journ., vol. 24, pp. 39-43. (In pp. 1-10. (In German.) Russian.) 90 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS 1949a. Atmospheric turbidity produced by 334 (in Russian). An English trans- the fall of the Tunguska meteorite lation appears in Soviet Astron. on June 30, 1908. Meteoritika, Journ., vol. 2, pp. 303-309, 1958. vol. 6, pp. 8-12. (In Russian.) The disintegration of asteroids produces Unusual atmospheric phenomena that a considerable amount of fine dust that occurred after the fall of the Tunguska spreads into space. To explain the ob- meteorite must have been caused by a served brightness of the zodiacal light, the large mass of thinly scattered material in density of this dust in the neighborhood of the atmosphere. For shorter wavelengths the earth must be 10"23 to 10~24 grams per (4000 to 7000 angstroms) the atmospheric cm3, as a lower limit. Good agreement transmission coefficients, determined at the exists between the observed form of the Mt. Wilson Station by the Smithsonian zodiacal light and the theoretical isophotes Astrophysical Observatory, showed a no- calculated (with the scattering fiinction of ticeable decrease in atmospheric trans- Piaskovskaia-Fesenkova) from the known parency from mid-July to mid-August, distribution of inclination angles of asteroid 1908, and some variation continued to orbits. This fact constitutes the strongest occur during the succeeding months. The argument in support of a meteoritic or author estimates the particles from the asteroidal origin for the zodiacal light. Tunguska meteorite to be of the order of 1/* in size, and the total mass to be at least 1959. On the nature of zodiacal light and a few million tons. its probable connection with aster- oids and periodic comets. Annales 1949b. The zodiacal light and the outer d'Astrophys., vol. 22, pp. 820-838. atmosphere of the earth. Russian The author gives a mathematical dis- Astron. Journ., vol. 26, p. 344. cussion of the nature of the zodiacal light Abstract in Astron. News Letter and its probable relation to asteroids and (Harvard), No. 54, p. 3, 1951. periodic comets. He shows that the ob- The author found an unsymmetrical served characteristics of the zodiacal light, distribution of the zodiacal light, which he including its polarization, can be accounted believes is not of cosmic origin but orig- for by the scattering of solar light by fine inates in an unsymmetric extension of the interplanetary particles, if their properties earth's atmosphere illuminated by the sun. are similar to those of aerosols always pres- ent in the upper atmosphere. No observa- 1950. On the gaseous tail of the earth. tions support the hypothesis that light is Russian Astron. Journ., vol. 27, scattered by free electrons. It is possible p. 89. Abstract in Astron. News to obtain the theoretical isophotes of the Letter (Harvard), No. 51, p. 8. zodiacal light from the distribution of the The author announces the discovery of inclinations of the orbits of periodic comets "false zodiacal light" seen in the western or asteroids. Periodic comets can account sky two or two and a half hours before for the observations, but an asteroidal sunrise, and probably related to the origin for the dust of the zodiacal light gegenschien. He discusses and rejects would require velocities of several kilom- Glyden and Moulton's meteoric hypothesis. eters per second for the dust, with respect The density of "tail" decreases by a factor to the parent asteroids. of two at intervals of 4.67 radii of the earth. FESSENKOFF, B. 1914. The zodiacal light. Gauthier-Villars, 1958. Zodiacal light as the product of disin- Paris, 174 pp. (In French.) tegration of asteroids. Russian Astron. Journ., vol. 35, pp. 327- FONTON, S. S. (see under Krinov and Fonton) ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 91 FREDERIKSSON, K. The author considers particles down to 1956. Cosmic spherules in deep-sea sedi- magnitude 30 (fine dust) and presents for- ments. Nature, vol. 177, pp. mulas for penetration if the particle speed is 32-33. high relative to the propagation of plastic Cores taken from the ocean bottom by deformation in the target. the Swedish Deep-Sea Expedition yielded several hundred black spherules greater GUTH, V. than 35jt in diameter, composed of metallic 1955a. Meteoric astronomy. Bull. Astron. iron nuclei surrounded by magnetite. The Inst. Czechoslovakia, vol. 6, pp. depth of the sedimentary layers in which 65-70 (in Russian); pp. 70-76 (in the spherules were found indicates a cosmic English); the abstract covers pp. origin. The estimated age of several mil- 75-76. lion years for the sedimentary layers indi- The author reviews Czechoslovakian cates that the spherules were probably work on meteoritic dust during the period deposited in the Tertiary Period. Spher- 1949 to 1955. ules obtained from atmospheric dust col- lected in Goteborg were found to be 1955b. Meteoritic dust. Transactions of the industrial in origin. Int. Astron. Union, vol. 9, pp. 303- 304. FREE, E. E. The author gives a short account of re- 1911. The movement of soil material by the search on meteoritic dust. He states that wind. U.S. Dept. Agriculture, L. Kresak has disproved the observation of Bureau Soils, Bull. 68, pp. 1-272. F. Link (1953) and Z. Linkova that the in- This paper includes a bibliography of tensity of the earth's shadow observed dur- Eolian geology, a discussion of extrater- ing lunar eclipses depends upon the amount restrial dust, numerous references to the of meteoritic dust in the atmosphere; literature of cosmic dust, and a discussion Kresak has shown that only very big me- of volcanic dust. teor showers could have any influence on the intensity of the shadow. Guth states GOODY, R. M. (see under Volz and Goody) that the question could be settled by opti- cal measurements of the brightness and GOSSNER, J. L. (see under Whipple and Gossner) polarization of the twilight sky.

GOTZ, F. W. P. HANDY, R. L., AND DAVIDSON, D. T. 1948. Some investigations at the Arosa 1953. On the curious resemblance between Light-Climatic Observatory touch- fly ash and meteoritic dust. Iowa ing solar-terrestrial relationships. Acad. Sci., vol. 60, pp. 373-379. Sixth Report of the Commission for the Study of Relations between The authors identify Thomsen's (1953) Solar and Terrestrial Phenomena, spherules as fly ash from coal-dust furnaces. Orleans, p. 166. HARTLEY, W. N., AND RAMAGE, H. "Bright nights" are probably associated 1901. The mineral constituents of dust and with an abnormal E-layer caused by in- soot from various sources. Proc. vasion of cosmic dust particles. Roy. Soc, London, vol. 68, pp. 97-109. See also abstract in Na- GRIMMINGER, G. ture, vol. 63, p. 552, 1901. 1948. Probability that a meteorite will hit or penetrate a body situated in the The dust that fell November 16, 17, vicinity of the earth. Journ. Ap- 1897, showed a regularity in composition plied Phys., vol. 19, pp. 947-956. and a similarity to meteorites in being 582933—61 2 92 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS magnetic and in having comparative free- rather than debris from larger bodies, and dom from extraneous matter. These thinks that the study of micrometeorites properties are in favor of its cosmic origin. can hardly fail to add to our knowledge of the origin and history of the solar system. HASEGAWA, I. 1956. Collecting and theories of meteoric HEIS, E. dust. Tenkai (The heavens), Orien- 1859. The meteorite spherules of Captain tal Astron. Assoc. Memoir No. 175, Callum. Wochenschr. Astron. Me- p. 226ff. (In Japanese.) Transla- teor. Geogr., new ser., vol. 2, p. tion of some sections into English, 319ff. (In German.) Reference Manual No. 1, Smith- A shower of small black spherules like sonian Astrophys. Obs., pp. 1-46, very fine shot fell on the American ship 1959. Joshua Bates, Nov. 14, 1856, about 60 miles The author describes methods of collect- southeast of Java. A small quantity was ing meteoric dust, gives details of various collected by Captain Callum for Lieutenant collecting projects in Japan, and reviews Maury, who sent a sample to Ehrenberg for previous work by others. He is interested microscopic study. Reported by Ehren- primarily in magnetic spherules. berg (1858). However, von Reichenbach (1859) regards these spherules as evi- HAWKINS, G. S. (see under Whipple and dence of a fireball. Hawkins) HIRST, W. P. HEARD, J. F. 1951. Some astronomical effects of radia- 1955. Meteorites large and small. Journ. tion. Monthly Notes, Astron. Soc. Roy. Astron. Soc, Canada, vol. 49, South Africa, vol. 10, pp. 44-46. pp. 49-63. The author discusses the effect of the An investigation was made of dust col- sun's radiation on small bodies, comets, lected by a filtering device operated in an and the zodiacal light. aircraft flying at an altitude of 6,000 feet in the Arctic. About 300,000 cubic feet of HODGE, P. air were filtered, producing 1950 particles. 1956. Opaque spherules in dust collected at Examination under a microscope of 100- isolated sites. Nature, vol. 178, power detected only two black spheres, in pp. 1251-1252. contrast to 36 collected by the same method above Windsor, Ontario, from air A preliminary report on dust collected subject to industrial pollution. This work simultaneously at three widely separated supports the conclusion of Hogg and Norris stations: in California, in central Alaska, in 1949 that such spherules have a ter- and in the Arctic. A detailed report ap- restrial origin. No bright metallic splin- pears in Hodge and Wildt (1958). ters were found, and the black spheres are probably not meteoritic. Assuming for AND RlNEHART, J. S. the particles a mean density of 3 gm/cm3, 1958. High-altitude collection of extrater- the author computes that at 6,000 feet the restrial particulate matter. Astron. Arctic air contained about 7 x 10~8 gm/ft3 Journ., vol. 63, p. 306. (Abstract.) of solid material at the time of the collec- The authors describe dust collected by tions. The magnetic fraction was 10 to millipore filters on jet aircraft flying at 100 times greater than the amount expected heights ranging from 20,000 to 55,000 from van de Hulst's calculations, and feet. The filters were examined with a probably only a small fraction was extra- high-power microscope. About 10,000 terrestrial. The author favors the theory particles were measured. Some dark that interplanetary dust is primordial shiny metallic particles may be extra- ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST

terrestrial, since their abundance does not 1932. Investigation of the zodiacal light. change rapidly with altitude, as with Veroff. Berlin-Babelsberg, vol. 10, particles of terrestrial origin. pt. 1, 141 pp. (In German.) The author associates the zodiacal light AND WILDT, R. with the concept of very small minor 1958. A search for airborne particles of planets. meteoritic origin. Geochim. et Cosmochim. Acta, vol. 14, pp. 1934a. On the cometary disturbances of the 126-133. upper layers of the atmosphere. Sitzungsber. Bayer. Akad. Wiss., The authors report on results of a year- Math-Nat. Abteil., pp. 129-144. long program involving daily collections of atmospheric dust at several widely 1934b. A hitherto unknown cosmic disturb- separated, isolated sites. The particles are ance in the upper atmosphere. Na- opaque shiny spherules with diameters less turwissenschaften, vol. 22, pp. 458- than 15/x, entirely different from the larger 460. spheres commonly found in densely popu- 1934c. Luminous bands, ionization of the lated areas. Their meteoritic origin is upper atmospheric layers and prop- suggested by recent evidence regarding agation of electromagnetic waves. ablation of meteorites, and by the fact that Forsch. u. Forschr., vol. 10, pp. the rate of fall and the frequency distri- 322-323. bution with size are the same at the several In the above three papers the author as- stations. The average rate of fall at each 2 serts that ionospheric disturbances as well station was 1.1 spherules per cm per day as luminous night-sky phenomena can with for particles greater than 3/z in diameter. a certain degree of assurance be attributed The rate of fall over the entire earth is 8 to cosmic disturbances or to intrusions of 5X10 kg per year. dust into the upper layers of the atmosphere. HOFFLEIT, D. 1949. Medal for meteor study awarded. 1934d. On the nature of the zodiacal light. Sky and Tel., vol. 9, p. 32. Pop. Astron., vol. 42, pp. 426-430. Note on F. L. Whipple's work on 1937. Meteors. Akademische Verlagsgesell- micrometeorites. schaft, Leipzig, chapters 2, and 3. (In German.) 1951. The Josiah and the Joshua Bates and This book contains material on inter- the meteoritic dust shower of stellar absorption, smoke trails, dust and November 14, 1856. Pop. Astron., ionization, ionization from dust-clouds of vol. 59, pp. 319-322. supposed cometary origin, the possibility The author clarifies the misconception that meteors and cosmic dust clouds might leading to the belief that there had been have influence on climate or weather, and two showers of dust, when in fact there had related topics. been only one. 1941. Remarks on the problem of the zodi- acal light. Astron. Nachr., vol. HOFFMEISTER, C. 271, p. 204ff. (In German.) 1930. Contribution to the photometry of the The author attempts to clarify the southern Milky Way and the reasons for the differences between the zodiacal light. Veroff. Berlin- terrestrial theory of F. Schmid and other Babelsberg, vol. 8, pt. 2, 60 pp. theories. (In German.) 1942. Remarks on the problem of the zodi- The author gives photographically deter- acal light. Astron. Nachr., vol. mined isophotes for the zodiacal light. 273, p. 131ff. (In German.) 94 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS 1951a. Interplanetary matter. Naturwiss., origin. The authors believe that some vol. 38, p. 227S. (In French.) extraterrestrial particles reach the earth's A semipopular article. surface but that identification would be difficult. 1951b. Specific luminous phenomena in the center of the ionosphere. Ergeb- HTTLBURT, E. O. nisse der exakten Naturwiss., vol. 1930a. A theory of zodiacal light. Phys. Rev., 24, p. Iff. (In German.) ser. 2, vol. 35, p. 663. (Abstract.) The author describes observed phenom- The paper presents a theory that assumes ena and interprets them in terms of micro- that the zodiacal light originates in the meteorites. uppermost layer of the earth's atmosphere. 1955. On some peculiar aspects of the 1930b. The zodiacal light and the gegen- zodiacal light. Mem. Soc. Roy. schein as phenomena of the earth's Sci. Liege, ser. 4, vol. 15, pp. 72-79. atmosphere. Phys. Rev., ser. 2, The author discusses some peculiar vol. 35, pp. 1098-1118. aspects of the zodiacal light and the gegenschein. He emphasizes that the zo- HULST, H. C. VAN DE diacal light is a topological or astrometric 1949. Scattering in the atmospheres of the problem, as well as a physical one. earth and the planets. In Kuiper, ed., The atmospheres of the earth HOGG, F. S. and planets, pp. 49-111. 1949. Meteoritic dust. Astron. Journ., vol. 1955. On the polarization of the zodiacal 54, p. 205. (Abstract.) light. Mem. Soc. Roy. Sci. Liege, The author outlines a program for col- ser. 4, vol. 15, pp. 89-95. lecting atmospheric dust and for extending The author discusses the polarization of the work to the Arctic. the zodiacal light. He explains that, con- 1950. Graduate work in meteoritic astron- trary to some claims, the polarization of omy and work on meteoritic dust the dust component may be appreciable in Canada. Letter to Professor and that an uncertainty in the electron Leonard, Pop. Astron., vol. 58, density arises from this fact. pp. 357-358. JAGER, C. DE The author discusses the search for 1955. The capture of zodiacal dust by the meteoritic matter in atmospheric dust, earth. Mem. Soc. Roy. Sci. Liege, and dust collecting in the Arctic. ser. 4, vol. 15, pp. 174-182. The author discusses the capture of zodi- HOPPE, J., AND ZlMMERMANN, H. acal dust by the earth. The amount of 1954. Separation of interplanetary from extraterrestrial dust observed on the earth industrial particles. Die Sterne, is about 103 times greater than the amount vol. 30, pp. 33-36. (In German.) computed from meteor frequencies. The The authors give a critical analysis of author suggests that for the zodiacal dust Thomsen's (1953) work. They show pic- the capture diameter of the earth is ap- tures of spherules obtained from iron proximately 8 x 106 km. The daily de- filings that had been passed through the posit of dust was computed on the basis of flame of a Bunsen burner, of steel chips, two different density distributions of the and of spherules produced by welding. zodiacal light. From van de Hulst's fig- Collections made at various distances ures the author found 1.6 x 103 kg per day, from the center of Jena suggest that and from Elsasser's he found 9.0 x 103 kg Thomsen's spherules were industrial in per day. ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 95

JUNG, B. diation. Proc. Indian Acad. Sci- 1939. Investigations of the zodiacal light. ences, "A," vol. 28, pp. 46-53. I: Gas and solid matter in the Spectrophotometric observations on solar system. Mitt. Univ. Stern- zenith-scattered light showed anomalous warte Breslau, vol. 5, p. 50ff. (In behavior, which is attributed to scattering German.) by large particles present in the atmos- The author discusses the motion of dust phere. particles in interplanetary space. KIZILIRMAK, A. KAISER, T. R., AND SEATON, M. J. 1954. Preliminary report on the amounts of 1955. Interplanetary dust and physical pro- iron dust which daily fall on the cesses in the earth's upper atmos- surface of the earth. Communica- phere. M6m. Soc. Roy. Sci. Liege, tions de la Faculty des Sciences de ser. 4, vol. 15, pp. 48-54. l'Universit^ d'Ankara, vol. 6, ser. The authors conclude that the density A, Fasc. 2, pp. 186-192. of interplanetary particles is too low for them to have much effect on the physical The author describes his collection of processes in the terrestrial upper atmos- irregular magnetic dust particles 1 to IOOJI phere, but that the particles probably ac- in length, found in and around Ankara. count for certain kinds of ionospheric Chemical analysis showed iron, but no abnormalities. nickel, cobalt, nor magnesium. The num- ber of iron particles that fell daily was re- KALLMAN, H. K. corded with the daily meteorological data. 1955. Quantitative estimate of frequency The iron dust may be terrestrial, the result and mass distribution of dust par- of erosion; or it may be extraterrestrial, ticles causing the zodiacal light from meteors. Some evidence indicates effect. M&n. Soc. Roy. Sci. Liege, that maximum particle counts occur on or ser. 4, vol. 15, pp. 100-113. near the days of meteor showers.

The author gives a quantitative esti- KLINE, B., AND BRIER, G. W. mate of frequency and mass distribution for dust particles that cause the zodiacal 1958. A note on freezing nuclei anomalies. light. She concludes that interstellar space Monthly Weather Review, vol. 86, has two classes of dust particles, with dif- pp. 329-333. ferent origins but similar densities: fast- The authors made daily observations of moving meteor particles and a quiescent freezing nuclei in the Washington, D.C., interplanetary dust cloud. area during the first three months of 1958. In spite of the probable observational un- KAMMERMAN, A. certainties, the fluctuations in the number 1886. Meteor shower of Nov. 27, 1885. of freezing nuclei were highly significant. Astron. Nachr., vol. 113, pp. 138- Near the January dates for which maxima 140. (In German.) were predicted by a meteoric dust hy- This paper deals with Yung's analysis of pothesis the values were abnormally high, the dust that fell on and after November 27 but later peaks do not seem to be associ- at Gent. A considerable number of me- ated with any known major meteor teoritic particles were found. streams. An analysis of the dates of marked peaks shown by similar observa- KARANDIKAR, R. V. tions made since 1954 at other places tends 1948. Effect of dust and haze on the spectral to confirm the presence of singularities in distribution of zenith-scattered ra- January which are statistically significant. SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

KOLOMENSKY, V. D., AND YuDIN, I. A. hi the atmosphere and comprises spheroidal 1958. The mineral composition of the fusion particles with diameters from a few microns crust of the Sikhote-Alin meteorite, up to 100/i. (2) Meteoritic dust is the and meteoritic and meteoric dust. product of the crushing of meteorites that Meteoritika, vol. 16, pp. 59-66. have fallen to the earth. The particles are (In Kussian.) small, acute-angled, irregular, and have a Sharp-edged particles from the dust con- composition and microstructure identical tain nickel-iron, magnetite, and iron hy- to those of meteorites. (3) Cosmic dust droxides (limonite and goethite). A few includes the smallest particles that invade spherical and rounded particles, both solid the earth's atmosphere from interplanetary and hollow, and from 0.2 to 0.04 mm in space; because of their small mass they size, resemble in mineral composition the reach the earth's surface practically unal- external zone of the fusion crust of the tered. They are Whipple's "micrometeor- larger meteorites, which consists mainly of ites." From examination of particles at oxymagnetite. The latter has a micro- the site of the Sikhote-Alin fall, the author granular structure with nodules of isome- concludes that particles of the dust trains tric form, 3 to 8/* in diameter. of bolides are solidified globules that are blown away from the melting surfaces of KRASOVSKY, V. I. meteoric bodies. He shows photographs 1946. Cosmic rays and the optical concen- of magnetic particles collected from the tration of scattered matter. Comp- site. They comprise primarily meteoritic tes Rendus, Acad. Sci., U.S.S.R., dust, plus a small number of globules with new ser., vol. 51, p. 183ff. (In diameters of 3/u to 800/z, as well as small Russian.) hollow flasks with open necks, and drop- Accepting as fact that iron and other shaped particles. metals in interstellar space have positive charges while stony particles have negative AND FONTON, S. S. charges, the author computes that a cloud 1952. Detection of meteoric dust at the of iron meteoritic particles of 10 a.u. radius place of fall of the Sikhote-Alin iron would have a potential of 3 x 1011 volts. meteorite shower. Doklady Acad. He then considers the charges that would Sci. Report, vol. 85, pp. 1227-1230. occur if the meteoritic cloud penetrated a (In Russian.) gas cloud. Charged particles with veloci- The particles of dust trains of bolides ties greater than 45 km per sec would seem to represent solidified droplet-globules release kinetic energy, possibly giving rise that are blown away from the melting sur- to the emission of cosmic rays. faces of meteoric bodies as they move with cosmic speeds and are spattered in the KRINOV, E. L. earth's atmosphere. Traces of the melted 1955. Basic meteoritics. State Publishing matter were found on the surfaces of the House of Technical-Theoretical Lit- Sikhote-Alin meteorites. Particles sub- erature, Moscow. (In Russian.) jected to fusion or those formed by the Translated by Irene Vidziunas and condensation of gasses may be spherules edited by Harrison Brown as Prin- and particles that are not affected by high ciples of meteoritics, Pergamon temperatures may be acute-angled. Press, 535 pp., 1960. The author describes dust found at the 1954. Meteoric dust from the place of fall site of fall of the Sikhote-Alin iron meteor- of the Sikhote-Alin iron meteorite ite. He favors the following classification shower. Meteoritika, vol. 11, pp. for extraterrestrial material: meteoric, me- 122-131. (In Russian.) teoritic, cosmic. (1) Meteoric dust results The authors present a table of the fre- from the disintegration of meteoric bodies quency of spherules and meteoritic particles ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 97

from samples of the soil at the Sikhote- LEONARD, F. C. Alin site. For another presentation of the 1941. Small aerolites recovered from the work, see Krinov (1952). site of the Holbrook, Arizona, fall of 1912. Pop. Astron., vol. 49, KULIK, L. A. pp. 384-386. 1926. On the question of the relation be- Aerolitic particles have been found in tween meteorites and comets. ant-hills; they weigh from 0.0074 to 0.0628 MirovedSnie", vol. 15, p. 173ff. (In gm. German.) The author discusses luminous night LEVI-CIVITA, T. clouds associated with the great Siberian 1930. Maxwellian distribution of cosmic meteorite fall. dust. Pont. Ace. Sci., N. Lincei, Atti, vol. 83, p. 176ff. LAEVASTU, T., AND MELLIS, O. Cosmic dust includes particles of all 1955. Extraterrestrial material in deep-sea sizes, even meteorites. If the distribution deposits. Trans. Amer. Geophys. is Maxwellian, the result of an encounter Union, vol. 36, pp. 385-389. with a planet is always directly opposed to The authors examined black spherules the planet's motion. from a Pacific Ocean core obtained by the Swedish Deep-Sea Expedition of 1947- LEVIN, B. J. 1948. They estimate that about 125 tons 1943. The nature of gas and dust trains of of black cosmic spherules fall on the earth various types. Russian Astron. each year and suggest that Pettersson and Journ., vol. 20, p. 49ff. (In Rus- Rotschi's (1952) chemical analysis gave too sian.) See also, Doklady Acad. Sci. Report, vol. 38, p. 304ff. large averages of NiO and Fe2O3 for the minute quantities of spherules present. 1955. Spatial density of interplanetary par- The authors conclude that nickel and iron ticles and their distribution accord- seem to be derived partly from coprecipita- ing to size. Me"m. Soc. Roy. Sci. tion from sea water. LiSge, ser. 4, vol. 15, pp. 114-124. (In French.) LANDSBERG, H. E. The author discusses the space density of 1947. A report on dust collections made at interplanetary particles and their distribu- Mount Weather and Arlington, tion in size. He concludes that at present Virginia, 1 October to 20 Novem- the astronomy of meteors and studies of ber, 1946. Pop. Astron., vol. 55, the zodiacal light and corona give only pp. 322-325. (Abstract.) uncertain data on the solid matter in Certain of the dust particles are thought interplanetary space. However, the study of interplanetary matter is important both to be of cosmic origiD. for astronomy and for the physical consti- LANE, A. C. tution of the earth. Hence, theoretical 1913. Meteor dust as a measure of geologic and observational studies should be carried time. Science, vol. 37, pp. 673- out by all means at our disposal. 674. 1956. Physical theory of meteors and mete- oric material in the solar system. LARMOR, J. Publishing House of the Academy 1938. Origins of the zodiacal light. Nature, of Sciences, Moscow, pp. 266-281. vol. 141, p. 201ff. (In Russian.) As origin, the author suggests a nebula The author discusses the results obtained surrounding the sun. by other investigators, and summarizes in 98 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS a table some values obtained by various effective diameter of particles that produce workers for the space density of meteoric the greatest absorption he obtains values material in the vicinity of the earth's of the order of one ft. A systematic, ex- orbit. He believes that a considerable tensive collection of meteoric dust could amount of meteoric material reaches the provide data on the nature of the particles earth's atmosphere not in the form of and their total mass. However, particles cosmic dust, but in the form of large porous that enter the earth's atmosphere simulta- bodies that disintegrate and evaporate in neously are not collected simultaneously the atmosphere. on the surface of the earth, since the time required to fall depends on their diameters. LIBEDINSKY, B. During a long time of fall, fine iron parti- 1933. Cosmic dust and noctilucent clouds. cles may be oxidized and therefore would Himmelswelt, vol. 43, p. 226ff. (In not be found in magnetic material collected. German.) 1955. The role of meteoric dust in the earth's This paper gives a general review and atmosphere. M6m. Soc. Roy. Sci. reaches a good many forced conclusions. Li6ge, ser. 4, vol. 15, pp. 35-47. It summarizes knowledge of noctilucent (In French.) clouds, the bright night clouds of June 30, 1908, and the Tunguska meteorite fall, and The author summarizes previous obser- attempts to show that the cosmic dust vational and theoretical research on mete- cloud which produces the bright nights and oric dust in the earth's atmosphere. the noctilucent clouds has a period of about 1956. On the amount of meteoric dust in the 6 years and is associated with the Pons- earth's atmosphere. Bull. Astron. Winnecke comet. It discusses Norden- Inst. Czechoslovakia, vol. 7, pp. skiold's description of meteoritic dust-fall. 69-75. (In French.) LINK, F. A difference of the order of 10 exists be- 1950. Optical soundings of the upper at- tween values for the amount of meteoritic mosphere with the help of lunar accretion deduced by direct determinations eclipses. Internat. Assoc. Terr. (Pettersson 1955) and by indirect measures Magn. Elect. Bull., no. 13, pp. 502- (Link 1953). To explain the difference 503. (In French.) Svestka thought it necessary to postulate Observations of the optical density of the meteoric particles with radii one tenth of a earth's shadow show it to be a function of micron or less, while the author suggested the distance from the center; and from a radius of one micron. Link believes photometric theory the density of the Svestka's arguments to be incorrect, and shadow can be calculated. The difference that it is preferable to retain the value of between the observed and the computed one micron and to look elsewhere for an ex- values increases rapidly from 24 km to the planation of the difference, if it is not top of the O8 layer. A further layer is simply the result of the inevitable errors in indicated at 100 km; it may be meteoric the methods employed. dust. LINKE, F. 1953. Meteoric dust in the earth's atmo- 1909-1910. Lectures: 2. Twilight phenom- sphere. Bull. Astron. Inst. Czech- ena, their regularities and disturb- oslovakia, vol. 4, pp. 158-161. (In ances. 3. Geophysical occurrences French.) during the earth's passage through The author considers the possibility that a comet's tail. 4. Preliminary geo- a high altitude layer of meteoritic dust physical results of observations of would cause absorption of light that could the passage of the comet from May be observed during lunar eclipses. For the 18-19 in Frankfort on the Main. ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 99 Jahresbericht des Physikalischen vol. Ill, pp. 268-277. See also Vereins zu Frankfurt am Main, abstract in Observatory, vol. 71, pp. 55-60. (In German.) p. 179. This paper discusses normal effects at The author considers comets as consist- twilight of dust in the atmosphere, the ad- ing of widely separated solid particles, some ditional effects that might be anticipated of which collide with one another at relative from the passage of Halley's comet, and velocities sufficient to pulverize them. The very briefly the effects actually observed. resulting particles of diameter of the order 6 1910. Aeronautical Meteorology, 126 pp. 10" cm are repulsed by solar radiation pressure to form the tails. The author mentions Halley's comet as a source of atmospheric dust, May 1910 (pp. MAPPER, D. (see under Smales, Mapper, and 40-45), and discusses the effect of sun- Wood) light on the diurnal variation of heights of dust-layers in the atmosphere, and optical MAYNE, K. I. phenomena from dust. 1956. Terrestrial helium. Geochim. et Cosmochim. Acta, vol. 9, pp. 174- AND OTT, J. 182. 1909-1910. Geophysical observations on the The amount of He4 released to the atmos- Feldberg i.T. during the passage of phere from the earth's crust is 60 times Halley's comet. Jahresbericht des greater than had previously been esti- Physikalischen Vereins zu Frank- mated. Because of the isotopic abundance furt am Main, pp. 98-126. (In ratio of atmospheric helium (He3/He*~1.2 German.) X10~fl), the production of He3 in the at- Observations of Bishop's ring indicate mosphere must be greater than the amount that dust penetrated deep into the atmo- calculated from (n, H3) reactions induced sphere but settled into the lower regions by cosmic rays on nitrogen. Extrater- only gradually (a matter of days). restrial dust, continuously received by the LOCK, C. (see under Packer and Lock) earth at the rate of 5,000 tons per day, is considered as a source of He3. The LYONS, J. B. (see under Stoiber, Lyons, El- author favors the theory that this is the berty, and McCrehan) interplanetary dust associated with the zodiacal light. He stresses the desirability LYTTLETON, R. A. of cosmic dust collection, particularly in 1948. On the origin of comets. Monthly Antarctica where one cubic meter of snow Notices Roy. Astron. Soc. London, should contain one milligram of cosmic vol. 108, pp. 465^75. dust. During the passage of the sun through a cloud of interstellar dust the particles MCCREHAN, R. H. (see under Stoiber, Lyons, converge to the accretion-axis where their Elberty, and McCrehan) transverse velocities are destroyed by col- MELLIS, O. (see under Laevastu and Mellis) lisions. A stream of dust forms at the axis, and for low relative speed of the sun MEUNIER, S. and cloud, that part of the stream within 1884. Dust, liquids, and gas of meteoritic several hundred astronomical units is origin. Chemistry Encyclopedia, captured and flows toward the sun. II, Metalloids, pp. 307-318. (In 1951. On the structure of comets and the French.) formation of tails. Monthly No- Treats various sources: earliest, Saloman, tices Roy. Astron. Soc. London, Hanover, Dec. 3, 1586; latest, Yung, 100 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS Switzerland, 1876. Also states, "Le navier at an international conference on Astro- Josiah-Bates naviguant, dans la nuit du 24 physics, held at Liege in July 1954. au 25 Janvier 1859." Cf. E. Heis (1859), who gives different dates; 1859 is wrong. MURRAY, J., AND RENARD, A. V. 1884. On the microscopic characters of 1903. Shower of dust recently observed in volcanic ashes and cosmic dust, and Iceland. Comptes Rendus, Paris, their distribution in the deep-sea vol. 136, p. 1713ff. (In French.) deposits. Proc. Roy. Soc. Edin- Red snow was observed the evening of burgh, vol. 12, p. 490ff. May 27 at latitude 64°54' N, longitude 13°40' E, and opaque black granules, some NEWKIRK, G. rounded, glassy, "des filaments et des 1959. Measuring variations in sky bright- globules." Similar dust fell in Norway ness. Naval Research Reviews, and Sweden in 1875, and was like Batavian October, pp. 20-22. tears. No polarization was observed. Preliminary measurements show that at Such material is probably produced sud- an altitude of 38,000 feet the daytime sky denly at temperatures below —100°. is five times brighter than it would be if the earth's atmosphere were free of contam- AND TlSSANDIER, G. inating dust. Measures were made by 1878. The presence of magnetic spherules, means of a coronograph flown in a high- similar to those of atmospheric altitude balloon. dust, in rocks of ancient geological periods. Comptes Rendus, Paris, NININGER, H. H. vol. 86, p. 450ff. (In French.) 1941. Collecting small meteoritic particles. Magnetic spherules collected from the Pop. Astron., vol. 49, pp. 159-162. air and the sea-bottom are compared with The author discusses the recovery of certain similar ones found in sands from gravel-size meteorites and the importance deep wells. of studying even finer dust.

MILLMAN, P. M. NORDENSKISLD, N. A. E. 1954. Meteor showers and rainfall. Journ. 1874a. On the cosmic dust which falls on the Roy. Astron. Soc. Canada, vol. 48, surface of the earth with the atmos- pp. 226-227. pheric precipitation. Philos. Mag., The theory that rainfall and meteor ser. 4, vol. 48, p. 546ff. showers are related confronts astronomical 1874b. On cosmic dust which falls with atmos- and geophysical difficulties that have not pheric precipitation on to the earth's been fully considered. Rainfall data for surface. Poggendorf, Annalen der the southern hemisphere (Bowen, 1953) Physik und Chemie, vol. 151, cannot be correlated with meteor showers in pp. 154-165. (In German.) the northern hemisphere. The rate of settling from the 100-km level will vary The author believes he has proved the greatly with the size of the meteoritic presence of cosmic dust by comparison with particles, and relatively sharp rainfall peaks analyses of other dusts collected from air. are difficult to explain. 1883. Program for the expedition to Green- land. Nature, vol. 28, p. 37ff. MINNAERT, M. From the collection of new data on cos- 1955. Dust in the interplanetary space. mic dust, the author believes there is M6m. Soc. Roy. Sci. Liege, ser. 4, greater variation in dust falls than is gen- vol. 15, pp. 15-34. erally assumed. The polar regions espe- The author introduces a series of papers cially are suited to a search for such on dust in interplanetary space, presented material. ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 101 1885. Studies and research instigated during earth's crust. Although the terrestrial my travel in the High North. Leip- abundances agree best with those of the zig, Brockhaus. (In German.) deep-sea deposits, this does not necessarily This paper is mostly devoted to the imply a terrestrial origin for the latter. author's theory of the vast importance of The earth's outer crust itself, being the last cosmic dust and contains much about addition to our planet from cosmic sources, meteors and meteorites as well as a list of may be built of a material whose remnants dust falls (p. 157). Pages 121-127 cover are still falling on the earth from the the geological importance of the fall of zodiacal-light cloud. cosmic dust on the earth's surface with 1956. Interplanetary dust and terrestrial special consideration of the theory of Kant accretion of meteoric matter. Irish and Laplace. Astron. Journ., vol. 4, pp. 84-135. 1894. On the great dust fall in Sweden and In a long and detailed discussion the adjacent lands on May 3, 1892. author considers a number of processes Met. Zeitschr., vol. 11, p. 212ff. of accretion and evaluates limits for par- (In German.) ticle sizes and amounts. The radius for metallic particles in interplanetary space The subsections present older observa- 6 tions of dust-showers, the various types, has a lower limit of 7.2 X 10~ cm because of radiation pressure. For compact stone dust of unquestionable cosmic origin, lists 5 of falls, and analyses. fragments the lower limit is 1.9X10" cm. Zodiacal dust is the main source of ter- OLEAK, H. restrial accretion, and direct collision is 1956-1957. The behavior of small meteoritic the most important process. With a particles in the earth's atmosphere. space-density of zodiacal dust of 2X10~21 Wiss. Zeitschr. Friedrich-Schiller gm/cm3, the total accretion is most probably Universitat, Jena, vol. 6, pp. 133- 0.051 grams in 106 years per horizontal 143. (In German.) square centimeter of earth's surface, or The author presents a mathematical dis- 250,000 tons of meteoric dust per year over cussion of the behavior of small meteoritic the entire surface of the earth. A table is particles (10~2 to 10~7 cm) in the atmos- included of the relative abundances of phere, and discusses their velocities as a nickel, cobalt, and copper. function of height, the height at which they begin free fall, the time of fall, and prob- OTT, J. (see under Linke and Ott) lems of ablation. OVENDEN, M. W. OPIK, E. J. 1951. Meteors and space travel. Journ. 1955. Cosmic sources of deep-sea deposits. British Interplanetary Soc, vol. 10, Nature, vol. 176, pp. 926-927. p. 176ff. The author gives a table (with references) Present observations indicate a negli- for various abundance ratios obtained for gible danger to an interstellar rocket of iron, nickel, cobalt, and copper. He sug- collision with interstellar dust particles. gests that the nickel of the deep sea may be of cosmic origin, even though other abun- PACKER, D. M., AND LOCK, C. dances in sea material differ from those 1950. The brightness and polarization of the of meteorites. There is no good reason to daylight sky at altitudes of 18,000 assume that abundances of elements in to 38,000 feet above sea level. cosmic dust would be identical with those Naval Res. Lab. Report 3713, in meteorites. Attention is called to the July 31. larger ratio of nickel to iron in cores from The data indicated the presence of large the Pacific, as compared with that in the scattering particles in the atmosphere above 102 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

the observers at all altitudes. Observa- PETTERSSON, H. tions were made from a B-29 over Arizona, 1949. Exploring the bed of the ocean. over southern California, and over western Nature, vol. 164, pp. 468-470. Canada, flying at 27,500 feet over snow This general article mentions tiny mete- fields and at 3,400 feet over cloud layer. oritic pellets as part of the deposit.

PALMIERI, P. 1955. Magnetic spherules and meteors. 1879. Studies of dust collected on February Naturwiss., vol. 42, pp. 387-388. 25, 1879 in Portici. Rend. R. Ace. (In German.) Sci. Fis. Naples, vol. 18, p. 112ff. The paper summarizes the results of (In Italian.) research on iron spherules collected by the Swedish Deep-sea Expedition of 1947- The author found Fe O by use of a 3 4 1948. The number of magnetic spherules magnet, but did not find Fe or efferves- collected from Pacific Ocean sediments cence with acids. (nearly 1,000 per kilogram of sediment) is 1901. On terrestrial and cosmic dust, and 20 to 40 times greater than the number the African sands. Analysis and previously found. The spherules occur to discussion. Rend. R. Ace. Sci. a depth of at least 3 meters under the Fis. Naples, ser. 3, vol. 7, pp. 156, sediment area, indicating a deposit age of 163, 172. (In Italian.) from 1.5 to 3 million years. The author gives the history of the fall 1960. Cosmic spherules and meteoritic dust. of March 10, 1901, and states that particles Sci. American, vol. 202, no. 2, of Fe3O4 were found. pp. 123-132. A plausible figure for the amount of PATON, J. meteoritic dust landing on the earth is 1951. Auroras and luminous night clouds. 5 million tons per year. The figure is Nature, vol. 168, pp. 487-488. based on the author's measures of deep-sea The nature and origin of the clouds are cores and of samples obtained in Hawaii, still uncertain. Meteoric dust would tend and on values given by other scientists. to drift to and remain below the base of the temperature inversion at 80 km. The — AND ROTSCHI, H. presence of the clouds at this level is in 1950. Nickel-content of deep-sea deposits. itself evidence for the existence there of a Nature, vol. 166, p. 308. temperature minimum. Preliminary results from the Swedish Deep-Sea Expedition of the Oceanografiska PENNISTON, J. B. Inst., Goteborg. If the nickel found is of 1931. Note on the origin of loess. Pop. meteoritic origin the apparent rate of Astron., vol. 39, pp. 429-430. accretion is estimated at several thousand tons a day, which is considerably more than The author proposes meteoric dust as the astronomers get on the basis of visual and origin. telescopic counts of meteors entering the 1942. Detailed description of the zodiacal atmosphere. light. Pop. Astron., vol. 50, pp. 1952. The nickel content of deep-sea de- 547-552. posits. Geochim. et Cosmochim. This paper, based largely on observa- Acta, vol. 2, pp. 81-90. tions by G. Jones during Perry's expedi- Determinations of the amounts of nickel, tion to Japan, 1853-1856, favors the theory manganese and iron present in sediment that zodiacal light is a ring or disc around cores from the central Pacific Ocean have the sun. been made by microchemical methods. ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 103

The nickel content in most cores was much REDMAN, R. O. higher than the average value for conti- 1959. Dust and gas between the earth and nental rocks and sediments, with maximum the sun. The Observatory, vol. 79, values ten times higher than the conti- pp. 172-181. nental average. The highest nickel values The distribution of gas and dust is fairly were found in material with a low rate of continuous between the sun and the earth. sedimentation (of the order of 1 millimeter Blackwell's photography from aircraft at in 1,000 years). eclipses, with subsequent measures and The authors found considerable variation analyses, has closed the gap between the with depth in the nickel content below the corona and the zodiacal light measures. sediment surface. No correlation with Evidence shows a variability of the zodiacal manganese and iron contents was evident light, which probably results from varia- except in places where a change in the rate tion in the number of electrons in the gas of sedimentation appears to have affected rather than from a changing amount of all three elements similarly. dust. Although satellite research, with The authors tentatively suggest that the measurements from places far beyond the abyssal nickel may derive partly from the moon, will be valuable in later years, the settling of cosmic dust over the earth's best optical techniques used either from surface. the ground or from conventional aircraft can still add to our present knowledge. PICH, R. (see under Schoenberg and Pich)

REICHENBACH, K. L. F. VON PIOTBOWSKI, S. L. 1952. The collisions of asteroids. Astron. 1859. Captain Callum's meteoric spherules. Journ., vol. 57, p. 23. [Poggendorf's] Annalen der Physik und Chemie, ser. 2, vol. 106, Several million tons of matter are pul- pp. 476-490. (In German.) verized to dust annually by collisions be- The author discusses meteoric dust from tween minor planets. This dust is thought the Joshua Bates, 1856, and argues against to replenish the dust of the zodiacal light Ehrenberg's volcanic theory to explain that slowly spirals into the sun. these spherules. He concludes that the Fe O dust of a great iron or iron-rich RAMAGE, H. (see under Hartley and Ramage) 3 4 meteor had fallen upon the deck of the Joshua Bates, and that the sample sub- RANYARD, A. C. mitted to Ehrenberg showed what the train 1878. On the presence of particles of iron in of such a meteorite consists of. the atmosphere. Astron. Regis- ter, vol. 16, pp. 299-300. RENARD, A. V. (see under Murray and Renard) This paper, abstracted as read at the meeting of the Royal Astronomical Society, REVELLE, R. R. Nov. 8, 1878, discusses Murray's deep-sea 1944. Marine bottom samples collected in magnetic globules, Nordenskiold's snow the Pacific Ocean by the Carnegie samples, Flight's experiments, and Ran- on its seventh cruise. Carnegie yard's observations on shipboard. Inst. of Washington, Publication No. 556, pp. 1-180. 1879. Note on the presence of meteoric dust in the atmosphere. Monthly One magnetic spherule was found in red Notices Roy. Astron. Soc. London, clay. The author quotes Murray on cosmic vol. 39, pp. 161-167. constituents. 104 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

RlCHTER, N. phere is of meteoric origin. This dust can 1955. Experimental investigations concern- easily be collected by simple methods. ing the illumination of clouds of Simultaneous observations in different re- reflecting particles. M6m. Soc. gions could eventually establish a correla- Roy. Sci. Liege, ser. 4, vol. 15, tion between the number of metallic pp. 80-88. particles collected and periods of meteoric The author investigated the illumination activity. If a sufficient quantity could be of clouds of reflecting particles by experi- collected, it might be submitted to chemical ments on small grains of various metals. analysis. 1938. Item 9 on meteoric dust. Transac- RINEHART, J. S. (see also under Hodge and Rinehart) tions of the Int. Astron. Union, 1957a. Distribution of meteoritic debris vol. 6, p. 160. (Abstract.) about the Arizona meteorite crater. The problem of the origin of metallic dust Smithsonian Contr. Astrophys., vol. deposited from the atmosphere or found in 2, pp. 145-160. the soil or on the ocean floor has recently The author systematically investigated attracted renewed attention. From 10-day the distribution of meteoritic dust and of collections of such dust made in July to bits and pieces of meteoritic material scat- October during the years from 1927 to 1936, tered in the soil around the Arizona L. Rudaux infers that magnetic particles Meteorite Crater, in order to fix the direc- were more plentiful at the beginning of tion of flight and the mass of the meteorite August, and finds another maximum at the that made the crater. end of August and in early September. In Seven hundred samples of soil were col- 1928 and 1933, copious deposits also oc- lected from an area of 80 square miles curred in October (Giacobinids). System- around the crater. Three types of strongly atic observations are desirable. magnetic material were separated from the soil: (1) particles of nickel-iron; (2) iron- RUDAUX, L. oxide particles; and (3) black shiny parti- 1930a. Meteors. L'Ulustration, vol. 88, p. cles, probably bits of magnetite. The 513ff. (In French.) author concludes that 12,000 tons of meteo- Magnetic dust-deposits are more abun- ritic material surround the crater in the form dant in the period of the year that is rich in of dust. He believes that the meteorite meteors. The number of such particles approached from a southwest direction and, does not increase proportionally with the when it hit the earth, pitched forward large very variable deposits of atmospheric dust. amounts of fragmented and molten At Donville the deposits are even more material. abundant when the wind blows constantly 1957b. A soil survey around the Barringer off the sea. Two days after the passage Crater. Sky and Tel., vol. 16, of a great bolide in September 1927, the pp. 366-369. fragments were so voluminous that they The author gives a popular presentation could be seen with the naked eye on the of the data given in Rinehart (1957a). receiving surface. The author thinks this tends to break down the distinction between ROTSCHI, H. (see under Pettersson and Rotschi) meteors and bolides.

ROY, F. DE 1930b. Meteors and the earth. Aerial dust. 1935. Report of Commission 22. Transac- La Nature, vol. 58, part 2, p. 439ff. tions of the Int. Astron. Union, vol. (In French.) 5, pp. 326-328, 373-374. In this general, illustrated article, the It is important to determine if the mag- author discusses magnetic particles of netic metallic dust present in the atmos- extraterrestrial origin. ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 105 1933. Magnetic particles collected after the SCHOENBERG, E. meteor shower of October 9. La 1941. On the position of the axis of the zodi- Nature, vol. 61, part 2, p. 436ff. acal light. Astron. Nachr., vol 272, (In French.) p. 25ff. (In German.) The author describes a meteor shower The author opposes Hoffmeister's views. followed by a dust shower. AND PICH, R. AND VAUCOULEURS, G. DE 1939. Investigations of the zodiacal light. 1952. Meteorites. Manuel Pratique d'As- Mitt. Univ. Sternwarte Breslau, tronomie, pp. 239-242. (In vol. 5, p. Iff. (In German.) French.) This paper presents a study based on Microscopic meteoritic particles or re- observations made in the tropics, and in- mains of their disintegration are continu- cludes a section on the height of the earth's ously received by the atmosphere, as proved atmosphere at which light scattering oc- by particles found abundantly on the snows curs. of high mountain summits or on polar glaciers. Small particles were especially SCHUSTER, A. numerous after the meteor shower of Oc- 1882. B.A.A.S. report of the committee on tober 9, 1933. meteoric dust. Nature, vol. 26, p. 488. (Abstract.) SANDIG, H. All the volcanic dust that the author had 1941. The spatial arrangement of the zodi- at his disposal was carefully examined acal light material. Astron. Nachr., under the microscope, and its appearance vol. 272, p. 1. found to be altogether different from the The author does not support Hoffmeis- supposed meteoric dust. The author ter's theory. agrees with Tissandier.

SCHEWICK, H. VAN SEARLE, A. 1939. Mass and density of the zodiacal light. 1899. The zodiacal light. Astrophys. Vierteljahrschrift Astron. Gesell- Journ., vol. 8, pp. 244-245. schaft, vol. 74, p. 233ff. (In Progress of knowledge of the subject German.) removes the difficulties attending the hypothesis that the zodiacal light is bight SCHLOSS, L. reflected from meteoritic dust forming a 1935. Meteoric dust. Pop. Astron., vol. part of the solar system. Lambert's 43, pp. 63-64. theory is found inapplicable. The author describes a first attempt at collecting meteoritic dust by means of a SEATON, M. J. (see under Kaiser and Seaton) magnet. SEELY, B. K. (see under Crozier and Seely) SCHMID, F. 1928. The zodiacal light, its nature and its SEN GUPTA, P. K. cosmic or terrestrial formation. 1954. Periodic influx of interplanetary dust Hamburg, 128 pp. (In German.) particles into the terrestrial at- 1940. New contributions to the problem of mosphere. Indian Journ. Mete- the zodiacal light. Astron. Nachr., orol. Geophys., vol. 5, pp. 272-276. vol. 270, p. 220ff. (In German.) The author gives a brief review of earlier Some inconsistencies might be explained papers relating to the influx of inter- if the zodiacal light were considered as part planetary dust particles to the terrestrial of the earth's atmosphere. atmosphere. He favors the theory that 106 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS solar corpuscular streams repeatedly push ooze, red clay, and oceanic rocks from the the particles towards the earth and con- Atlantic, Pacific, and Indian Oceans, the centrate them near the earth and in the authors found that meteoritic material ecliptic. made little significant contribution to deep- sea sediments, unless some remarkable SIEDENTOPF, H. (see under Behr and Sieden- differential behavior of the three elements, topf) nickel, cobalt, and copper, has taken place.

SLIPHEB, V. M. SPENCER, L. J. 1931. A preliminary note on the spectrum 1933. Meteoric iron and silica glass from the of the zodiacal light. Lowell Ob- meteorite craters of Henbury (Cen- servatory Circular, February 20. tral Australia) and Wabar (Arabia). The author obtained spectra with dis- Mineralog. Mag., vol. 23, pp. 387- persion 6 mm from H to K. Keflected sun- 404. light with superposed emissions suggests Spherical particles resembling meteoritic that the zodiacal light arises in part in the dust were found. earth's atmosphere.

SLOCUM, F. STAUDE, N. 1934. Iridescent clouds and cosmic dust. 1923. On the astronomical theory of mete- Journ. Roy. Astron. Soc. Canada, ors. Astron. Nachr., vol. 218, p. vol. 28, pp. 145-148. 155ff. (In German.) The author discusses the daily variation SHALES, A. A.; MAPPER, D.; AND WOOD, A. J. in the brightness of the night sky on the 1958. Radioactivation analysis of "cosmic" basis of the meteoritic hypothesis for the and other magnetic spherules. zodiacal light. There are comments by C. Geochim. et Cosmochim. Acta, vol. Hoffmeister. 13, pp. 123-126. By neutron activation analysis, the STOIBER, R. E.; LYONS, J. B.; ELBERTY, W. T.; authors found the chemical content of AND MCCREHAN, R. H. magnetic spherules to lie in the range 0.03 1956. The source area and age of Ice-Island to 3.9 micrograms for nickel, 0.01 to 0.3 T-3. Final Report under Con- micrograms for cobalt, and 0.0006 to 0.53 tract AF19(6O4)-1O75, Dartmouth micrograms for copper. From the ratios College, Department of Geology. of nickel to copper, nickel to cobalt, copper to cobalt, and nickel to iron, two samples The authors identified magnetic sphe- from deep-sea cores are identified as being rules found in deep cores in Arctic Ice- closely related to iron meteorites. A sam- Island T-3 as probably extraterrestrial. ple from the roof of a station off the coast The composition was magnetite and the of Sweden and another from sand of the surfaces were sometimes striated. Particle River Danube have quite different chemi- size ranged from 5 to 100M and more. cal compositions. STRUVE, O. AND WISEMAN, J. D. 1943. Recent progress in astrophysics: V. G. 1955. Origin of nickel in deep-sea sediments. Fesenkov's dynamical theory of Nature, vol. 175, pp. 464-465. the zodiacal light. Astrophys. Journ., vol. 98, pp. 129-130. The ratios of nickel to cobalt, nickel to copper, and copper to cobalt are 13.1, 92, 1951a. Dust in the solar system. Sky and and 0.14 for meteorites, and 3.5, 1.1, and Telescope, vol. 10, pp. 88-91. 3.0 for igneous rocks. Using radioactiva- The author gives a general review of tion methods on samples of globigerina relevant current literature. ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 107

1951b. Photography of the counterglow. THIESSEN, G. Sky and Telescope, vol. 10, pp. 1948. Associations between the solar corona 215-218. and the zodiacal light. Himmel- In addition to describing the wide angle swelt, vol. 55, p. 161ff. (In Ger- equipment constructed by Greenstein and man.) Henyey, Struve reviews the theory by The interplanetary dust-cloud is dis- Fesenkov that the gegenschein or "false cussed. zodiacal light" is the earth's tail. He also presents the arguments of M. G. Karimov THOMSEN, W. J. and of N. B. Divari opposing this view. 1953. The annual deposit of meteoritic dust. Sky and Telescope, vol. 12, pp. SVESTKA, Z. 147-148. 1950. A note on the brightness of lunar The author collected magnetic spherules eclipses. Bull. Astron. Inst. Czech- from rooftops and buckets in Iowa City. oslovakia, vol. 2, pp. 41-43. He assumed that they were meteoritic. The author discusses the variation of the Spectroscopic analysis of the magnetic brightness of lunar eclipses with respect to spheres showed iron, silicon, and mag- an atmospheric dust layer. An earlier nesium. A gravimetric check gave SiO2, theory of a yearly periodicity is replaced 28 percent; Fe2O3, 72 percent. No nickel by the theory that the brightness may was detected. The spheres were 8 to 80/x depend in part on the quantity of meteoric in diameter. The rate of fall was cal- dust in the earth's atmosphere. culated to be 2 X 109 kg/yr for the entire 1954. The problem of a meteoritic dust earth. layer in the earth's atmosphere. TISSANDIEB, G. (see also under Meunier and Bull. Astron. Inst. Czechoslovakia, Tissandier) vol. 5, pp. 91-98. 1875. On the existence of iron and magnetic The author discusses again the evidence particles in atmospheric dust. for a high atmosphere dust layer, as Comptes Rendus, Paris, vol. 81, deduced from lunar eclipse observations. p. 576ff. (In French.) He calculates that only particles of radius The author concludes that some mag- 10~5 or 10~8 cm are consistent with the netic particles are not terrestrial in origin. observations. Such small particles would have to be carried to the lower parts of the TROWBRIDGE, C. C. atmosphere much faster than the rate 1907. Physical nature of meteor trains. computed for a quiet atmosphere. The Astrophys. Journ., vol. 26, pp. 95- author believes that turbulence could do 116. this. Meteor trains are self-luminous gas SWINGS, P. clouds combined with very minute me- 1949. The spectra of the night sky and the teoric dust particles; the latter in daylight aurora. In, Kuiper, ed., The at- reflect light like ordinary clouds. mospheres of the earth and planets, TSCHERKASS, W. K. (see under Tscherwinsky pp. 159-212. and Tscherkass)

THERNOE, K. TSCHERWINSKY, P. N., AND TSCHERKASS, W. K. 1941. The zodiacal light. Nordisk Astron. 1929. On why it is so difficult to prove the Tidsskrift, vol. 22, pp. 73-80. (In presence of cosmic dust on the sur- Danish.) face of the earth. Mirov6d6ni6, The author discusses various problems vol. 18, No. 2; Centralblatt Min. of the zodiacal light. Geol. Pol., Abt. A, pp. 127-129. 108 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS The authors compute that only 0.00007 measure the absolute intensity of the twi- milligram of meteoritic dust falls per square light in five narrow bands of wavelengths meter, annually. from the red to the ultra-violet region of the spectrum. Gradients of the logarithm VAETH, J. F. of intensity and color ratios give complex 1951. 200 miles up (the conquest of the but sensitive indicators of dust scattering, upper air). New York, 207 pp. which is small but measurable if precise The author discusses atmospheric dust absolute methods are used. The problem on pages 24-25 and 67. is very complex, but the authors think that useful information can be obtained up to VAUCOULEURS, G. DE (see under Rudaux and de 120 km for observations in blue light, and Vaucouleurs) up to 75 km for observations in red light.

VEGARD, L. WATSON, F. G. 1923a. The constitution of the upper strata 1956. Between the planets. Ed. 2, Cam- of the atmosphere. Philos. Mag., bridge. vol. 46, p. 557ff. WEIL, M. The author assumes a dust atmosphere 1922. Theories on the nature of meteor above the gaseous atmosphere, the gaseous trains, with a note on Professor ending at about 80-100 km above the Trowbridge's contributions to our surface, with the dust comparatively dense knowledge of meteor trains. Pop. at 100-120 km, slowly decreasing upward. Astron., vol. 30, pp. 524-535. 1923b. Distribution of matter in the highest The paper gives a historical bibliography, strata of the atmosphere. Videns- including references to reflection and other kapsselskapets Skrifter, Mat.- theories that assume meteor trains are com- Naturv. Klasse (Kristiania), no. posed of cosmic dust or a disintegrated 10. meteoroid. The author discusses nitrogen dust in WHIPPLE, F. J. W. the upper atmosphere, the tendency for 1934. Phenomena related to the great Sibe- electrified dust to drift toward the mag- rian meteor. Journ. Roy. Mete- netic equator, and the bearing of his orol. Soc, vol. 60, pp. 505-513. theory on the interpretation of the zodiacal light and gegenschein. Concerning the illumination of the sky on the nights following the arrival of the 1923c. On the constitution of the upper layers meteor, the author suggests that the meteor of the atmosphere. Comptes Ren- had a tail that was captured by the earth's dus, Paris, vol. 176, p. 1488ff. (In atmosphere. French.) WHIPPLE, F. L. This paper discusses nitrogen dust in the 1949. Report of Commission 22. Transac- highest layers of the atmosphere, and its tions of the Int. Astron. Union, vol. bearing on color changes along the paths 7, pp. 240-244. of meteors. Meteoritic dust has been collected by VOLZ, F., AND GOODY, R. M. H. H. Nininger and H. E. Landsberg, and 1960. Twilight intensity at 20° elevation. its consequences considered theoretically Scientific Report No. 1, pp. 1-46, by J. Kaplan and A. R. Khan. on Air Force Contract AF19- 1951a. Comets and the zodiacal light. 604(4546), Blue Hill Meteorological Astron. Journ., vol. 56, p. 51. Observatory, AFCRC-TN-60-284, (Abstract.) 1960. The icy-conglomerate model of comets, The authors designed a photometer to coupled with the Poynting-Robertson effect ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 109 and planetary perturbations, provides the corona and the zodiacal light. According required rate of addition of material to to the Poynting-Robertson effect, the the zodiacal cloud and also predicts the zodiacal cloud needs for its maintenance required distribution of particle sizes. about 1 ton/sec of small particles in the 4 1951b. Origin of the zodiacal light. Sky and 10~ to 1.0 cm range. Comets continu- ously contribute some 30 tons/sec. They Tel., vol. 10, p. 94. lose matter by the following four physical The author suggests that particles are forces or processes: (1) interstellar wind, blown off comets when icy surfaces of the (2) Jupiter's random perturbations, (3) the comets vaporize in sunlight; the particles Jupiter perturbation barrier, and (4) col- then spiral around the sun to form the zo- lisional destruction. The first and fourth diacal light. of these seem to be the most important. 1952a. Report of Commission 22. Trans. Int. Collisions among the particles seem to be Astron. Union, vol. 8, pp. 293-300. most responsible for the cutoff in zodiacal particle size above 0.03 cm, as found by Work in Czechoslovakia included in- van de Hulst. vestigation by M. Plavek on the Poynting- Robertson effect, the age of showers, and If it is great enough, corpuscular radia- the dimensions of comets; Link studied tion may be more important than the the concentration of meteoritic dust falling Poynting-Robertson effect; it may also re- through the atmosphere. In Japan, Huru- quire more material for the zodiacal cloud. hata carried out investigations on the light If this is true, corpuscular radiation will of the night sky and the zodiacal light; increase the critical cutoff dimension. he found a relation between the zodiacal 1955b. On the origin of the zodiacal particles. light and Comet Encke, and between the Me'm. Soc. Roy. Sci. Ltege, ser. 4, zodiacal light and the solar corona. In vol. 15, pp. 183-184. the U.S.S.R., Fesenkov's work on meteor- itic matter in interplanetary space dealt The author states that the Poynting- Robertson effect requires approximately also with the zodiacal light. Astapovich 4 and Khvostikov studied noctilucent clouds one ton/sec of small particles 10~ to 1.0 cm and found that they are not caused by in diameter to maintain the zodiacal cloud. meteoritic dust but by condensation of Consideration of the effect of corpuscular water vapor. radiation may indicate a considerably larger source of material for the zodiacal 1952b. Results of rocket and meteor research. cloud. The probable contribution to the Bull. Amer. Meteorol. Soc, vol. 33, zodiacal cloud from comets is considered pp. 13-25. on the basis of the icy comet model. This paper discusses the pitting of shiny 1958. The meteoric risk to space vehicles. surfaces of rockets probably by micro- Proc. 8th Int. Astronaut. Congr. meteorites, and the possibility of their con- Barcelona, 1957, pp. 418-428. tributing to E-layer ionization, light scat- tering, and twilight sodium radiation. The author discusses the distribution and rate of fall of meteoritic material as func- 1955a. A comet model. III. The zodiacal tions of mass and velocity, and presents light. Astrophys. Journ., vol. 121, a table concerning meteoroids and gives pp. 750-770. formulas for computing the probabilities of The author considers the probable com- penetration in space vehicles. The author etary contributions to the zodiacal cloud calculates upper limits for the effects of on the basis of the icy-comet model. He erosion on a space-exposed surface subject assumes the zodiacal cloud to be of the to erosion by meteoritic dust, corpuscular nature deduced by van de Hulst and Allen radiation from the sun, and gases of the from their studies of the Fraunhofer extended solar corona. He concludes that 110 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS the corrosive effect from meteoritic dust is of micrometeorites under the influence of comparable to the combined effects from corpuscular radiation from the sun. The the other two factors. rate of orbital spiralling is calculated to 1959. Solid particles in the solar system. be 15 times greater than that due to the Journ. Geophys. Res., vol. 64, light pressure component of the Poynting- pp. 1653-1664. Robertson effect. To affect amounts of rainfall, more cometary material than was The author discusses the present state originally postulated to supply the zodiacal of our knowledge concerning solid particles cloud would be necessary. in the solar system. Our best information comes primarily from studies of optical WILDT, R. (see under Hodge and Wildt) meteors, radio meteors, the zodiacal cloud and meteorite analysis. Both space obser- WISEMAN, J. D. (see under Smales and Wise- vations and ground-based experiments are man) important for the future. The author believes that 70 to 90 percent of the WOOD, A. J. (see under Smales, Mapper, and expected results from meteoritic studies can Wood) be provided from the ground, but such observations cannot give good information YAGODA, H. on solid particles in space much beyond 1959. Observations on nickel-bearing cosmic 1 a.u., and unexpected results may come dust collected in the stratosphere. from space observations. Geophysics Research Directorate Detailed knowledge of particles in the Research Notes No. 9, AFCRC- solar system is of practical importance to TN-59-200, ASTIA Document No. designers of space equipment and to AD-212422, pp. 1-13. operational planners. Theoretically, mete- The author used microchemical methods oritic material can provide basic informa- to examine stratospheric dust particles tion on the evolution of the earth and the collected on four balloon flights at altitudes solar system. He discusses possibilities for between 77,000 and 112,000 feet. Collec- meteorite instrumentation in space vehicles. tions were made on simple plastic dishes mounted at the top of the balloon and at AND GOSSNER, J. L. the gondola level, with continuous ex- 1949. An upper limit to the electron density posure at both levels. The preliminary near the earth's orbit. Astrophys. data showed that the relative abundance Journ., vol. 109, pp. 380-390. of nickel-bearing dust ranged between 0.17 Brightness and polarization observations and 0.36 particle per cm2 of collection are used. Observed polarization can prob- surface per day of exposure. Most of the ably be accounted for by the reflection of color reactions for nickel were given by sunlight by dust particles. particles of diameters between 20 and 40M, but positive reactions were also given by —AND HAWKINS, G. S. smaller particles with diameters of 1 to 2ju. 1956. On meteors and rainfall. Journ. Mete- orol., vol. 13, pp. 236-240. YAMAMOTO, I. The authors consider the role of micro- 1938. Report of the sub-commission on meteorites that enter the atmosphere with- zodiacal light. Trans. Int. Astron. out producing detectable light or ionization. Union, vol. 6, pp. 172-175. A large number of micrometeorites in a The author summarizes theories on the stream could affect rainfall. To explain nature of the zodiacal light by Hoffmeister, the removal of particles from the stream Schmid, Brunner, Larmor, and Donitch, the authors suggest a mechanism that and brings out the major differences in depends upon the gradual disintegration these theories. ANNOTATED BIBLIOGRAPHY ON INTERPLANETARY DUST 111

YAVNEL, A. A. The paper describes the great snowfall 1957. Meteoritic matter at the place of fall of Wednesday, December 5, 1883, at of the Tunguska Meteorite. Rus- Geneva. The author notes that fine me- sian Astron. Journ., vol. 34, pp. tallic dust is prevalent after the times of 794-796. (In Russian.) English meteor showers and believes the dust is due translation by F. W. Wright and to the rupture of a large meteorite and to P. W. Hodge, Tech. Rep. No. 7, microscopic meteorites. AF18(6OO)-1596, ASTIA Docu- ment No. AD 154 146, 1958. ZACHAROV, I. The author gives results of investiga- 1952. Influence of the Perseids on atmos- tions of the magnetic portion of soil pheric transparency. Bull. Astron. samples collected in 1927 to 1930 at the Inst. Czechoslovakia, vol. 3, pp. place of fall of the Tunguska meteorite. 82-85. (In French.) Visual examination with a microscope Measures of the darkness and size of the showed small metallic particles and black earth's shadow during lunar eclipses show shiny globules of magnetite, 30 to 60/x in that after the appearance of several of the diameter. Spectroscopic analysis showed most active meteor streams, our atmos- that the particles are composed of nickel- phere is polluted in the upper region by iron. The author concludes that these dust. These are either interplanetary dust particles are part of the Tunguska mete- particles or the residue of meteors, which orite, which was evidently an iron. The dissipate at 80 to 150 km. The author data show a great similarity with those for uses limited Mt. Wilson measurements to the Sikhote-Alin meteorite, as determined show that a slight decrease in the amount by Krinov and Fonton (1952, 1954). of atmospheric transparency follows a me- teor shower. The relatively short duration YoKOYAMA, E. of the depression is inconsistent with the 1950. Interim report on observations of at- time of fall of the particles. This discrep- mospherics which may be caused ancy is explained by the agglomeration of by meteoric showers. Proc. Imp. particles, which diminishes their absorbing Acad. Tokyo, vol. 6, p. 154ff. power and increases the speed of fall. The pollution of the atmosphere has a maxi- YUDIN, I. A. (see under Kolomensky and mum duration of 24 days. Particles with Yudin). diameters less than 0.1/u and of density 4 YUNG, E. would fall for some tens of years. 1883. A fall of cosmic dust. Comptes Ren- dus, Paris, vol. 97, p. 1449ff. (In ZIMMERMANN, H. (see under Hoppe and Zim- French.) mermann)