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4.8 Evolution and Detectability of Interplanetary Dust Streams

Published online by Cambridge University Press:  12 April 2016

Lubor Kresák
Lubor Kresák*
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, Bratislava, Czechoslovakia

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Sudden enhancements in responses recorded by micrometeoroid detectors flown on spacecrafts have been repeatedly attributed to encounters with streams of cometary debris similar to, or identical with, the meteor streams known from ground-based observations. Por measurements made in the Earth-Moon environment, spacecraft effects, atmospheric fragmentation of larger particles, and possibly lunar ejecta can be misinterpreted as interplanetary streams. For deep space observations it is necessary to inquire whether a compact dust stream can persist under the dispersive and destructive effects which increase rapidly with decreasing particle size.

Type
4 Meteors and their Relation to Interplanetary Dust
Information
International Astronomical Union Colloquium , Volume 31: Interplanetary Dust and Zodiacal Light , 1976 , pp. 391 - 395
Copyright
Copyright © Springer-Verlag 1976

References

Alexander, W.M., Arthur, C.W., Corbin, J.D. and Bohn, J.L. (1970). Space Research 10, 252.Google Scholar
Ashworth, D.G. and McDonnell, J.A.M. (1974). Space Research 14, 723.Google Scholar
Belton, M.J.S. (1967). In: The Zodiacal Light and the Interplanetary Medium. NASA SP-150, p. 301.Google Scholar
Berg, O.E. and Gerloff, U. (1971). Space Research 11, 225.Google Scholar
Harwit, M. (1963). J. Geophys. Res. 68, 2171.Google Scholar
Harwit, M. (1967). In: The Zodiacal Light and the Interplanetary Medium. NASA SP-150, p. 307.Google Scholar
Hemenway, C.L., Erkes, J.W., Greenberg, J.M., Hallgren, D.S. and Schmalberger, D.C. (1973). Space Research 13, 1121.Google Scholar
Kresák, L. (1966). Bull. Astron. Inst. Czech. 17, 188.Google Scholar
Kresák, L. (1968). In: Physics and Dynamics of Meteors. IAU Symp. 33, p. 391.Google Scholar
Levin, B.Yu. and Simonenko, A.N. (1972). Kosmicheskie Issledovaniya 10, 113.Google Scholar
Marsden, B.G. (1967). Astron. J. 72, 1170.Google Scholar
McDonnell, J.A.M. and Ashworth, D.G. (1972). Space Research 12, 333.Google Scholar
Millman, P.M. (1970). Space Research 10, 260.Google Scholar
Paddack, S.J. (1969). J. Geophys. Res. 74, 4379.Google Scholar
Radzievskij, V.V. (1954). Dokl. Akad. ÏTauk SSSR 97, 49.Google Scholar
Soberman, R.K. (1971). Rev. Geophys. Space Phys. 9, 239.Google Scholar
Wehner, G.K., KenKnight, C.E. and Rosenburg, D.L. (1963). Planet. Space Sci. 11, 885.Google Scholar
Whipple, P.L. (1967). In: The Zodiacal Light and the Interplanetary Medium. MSA SP-150, p. 409.Google Scholar
Wyatt, S.P. and Whipple, F.L. (1950). Astrophys. J. 111, 134.CrossRefGoogle Scholar
Zook, H.A. and Berg, O.E. (1975). Planet. Space Sci. 23, 183.Google Scholar