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On the Amount of Dust in the Asteroid Belt

Published online by Cambridge University Press:  12 April 2016

Fred L. Whipple
Fred L. Whipple*
Affiliation:
Smithsonian Astrophysical Observatory and Harvard College Observatory

Abstract

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Calculations of upper limits to the quantity of small particles in the asteroid belt are based on (1) the brightness of the counterglow coupled with observations and theory for the zodiacal cloud near Earth's orbit and (2) the destruction and erosion of asteroidal particles as they spiral toward the Sun because of solar radiation via the Poynting-Robertson effect. These calculations place the likely upper limit on asteroidal space particle density at the order of 5 to 10 times and the hazard to space vehicles at 2 to 4 times those near Earth's orbit. No such evidence indicates, however, that the hazard from small particles is actually much greater in the asteroid belt.

Type
Part II-Origin of Asteroids Interrelations with Comets, Meteorites, and Meteors
Information
International Astronomical Union Colloquium , Volume 12: Physical Studies of Minor Planets , 1971 , pp. 389 - 393
Copyright
Copyright © NASA 1971

References

Allen, C.W. 1963, Astrophysical Quantities, p. 145. Athlone Press. Univ. of London.Google Scholar
Crozaz, G., Haack, U., Hair, M., Maurette, M., Walker, R., and Woolum, D. 1970, Nuclear Track Studies of Ancient Solar Radiations and Dynamic Lunar Surface Processes. Proc. Apollo 11 Lunar Sci. Conf. Geochim. Cosmochim. Acta 34, Suppl. 1, vol. 3, pp. 2051–2080.Google Scholar
Dohnanyi, J.S. 1967, Mass Distribution of Meteors. Astrophys. J. 149, 735–737.Google Scholar
Dohnanyi, J.S. 1969, Collisional Model of Asteroids and Their Debris. J. Geophys. Res. 74, 2531–2554.CrossRefGoogle Scholar
Dohnanyi, J.S. 1970, On the Origin and Distribution of Meteoroids. J. Geophys. Res. 75, 3468–3493.Google Scholar
Ganapathy, R., Keays, R.R., and Anders, E. 1970, Apollo 12 Lunar Samples: Trace Element Analysis of a Core and the Uniformity of the Regolith. Science 170, 533–535.Google Scholar
Hörz, F., Härtung, J.S., and Gault, D.E. 1970, Micrometeorite Craters on Lunar Rock Surfaces. Lunar Sci. Inst. Contrib. no. 9.Google Scholar
Keays, R., Ganapathy, R., Laul, J.C., Anders, E., Herzog, G.F., and Jeffery, P.M. 1970, Trace Elements and Radioactivity in Lunar Rocks: Implications for Meteorite Infall, Solar-Wind Flux and Formation Conditions of Moon. Science 167, 490–493.Google Scholar
Robertson, H.P. 1937, Dynamical Effects of Radiation on the Solar System. Mon. Notic. Roy. Astron. Soc. 97, 423–438.Google Scholar
Roosen, R.G. 1969, The Gegenschein. Doctoral Dissertation, Univ. of Texas.Google Scholar
Roosen, R.G. 1971, Earth’s Dust Cloud. Nature 229, 478–480.Google Scholar
Whipple, F.L. 1967, On Maintaining the Meteoritic Complex. The Zodiacal Light and the Interplanetary Medium (ed., Weinberg, J.L.), NASA SP-150, pp. 409–426.Google Scholar