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6. The Nature of Asteroid Surfaces, from Optical Polarimetry

Published online by Cambridge University Press:  12 April 2016

A. Dollfus ,
J. E. Geake ,
J. C. Mandeville  and
B. Zellner

Abstract

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Telescopic observations of the polarization of light by asteroids are interpreted on the basis of a systematic polarimetric analysis of terrestrial, meteoritic and lunar samples. Laboratory measurements were made using samples with different surface textures, and scanning electron microscope pictures were used to investigate the influence of microtexture and crystalline structure.

It is demonstrated that asteioid surfaces do not accumulate thick regolithic layers of micro-fragments, as do the Moon and Mercury. This is because the majority of debris ejected by impacts are lost, due to the low gravitational escape velocity from these bodies. However, asteroids are not bare rocks, but are coated with a thin layer of adhesive debris. This coating apparently has the composition of the body itself. The fact that there is no indication of significant maturation by space weathering suggests that the dust which coats the surface of asteroids is frequently replaced by further impacts.

Asteroids may be classified polarimetrically in several groups: those in group C are made of very dark material and behave like carbonaceous chondrites, or very dark Fe-rich basalts; Those in group S correspond to silicates and stony meteorites. A third group represented by Asteroid 21 Lutetia and 16 Psyche may be metallic.

Type
Part IV. Physical Nature of Asteroids
Information
International Astronomical Union Colloquium , Volume 39: Comets, Asteroids, Meteorites: Interrelations, Evolution and Origins , December 1977 , pp. 243 - 251
Copyright
Copyright © A.H. Delsemme 1977

References

Adams, J. B., and McCord, T. B. 1971, Proc. Second Lunar Science Conf., 3, 2183–2195.Google Scholar
Arrhenius, G., and Asunmaa, S. K. 1973, The Moon, 8, 368–391.CrossRefGoogle Scholar
Bowell, E., Dollfus, A., Zellner, B., and Geake, J. E. 1973, Proc. Lunar Science Conf. 4th, 3167–3174.Google Scholar
Chapman, C., Morrison, D., and Zellner, B. 1975, Icarus, 25, 104.CrossRefGoogle Scholar
Dohnanyi, J. S. 1971, NASA-SP-267.Google Scholar
Dollfus, A. 1971, in Physical Studies of Planets, Gehrels, T., Editor, NASA-SP-267, pp. 95–116.Google Scholar
Dollfus, A., and Geake, J. E. 1975, Proc. Lunar Sci. Conf. 6th, 2749–2768.Google Scholar
Duraud, J. P., Langevin, Y., Maurette, M., Comstock, G., and Burlingame, A. L. 1975, Proc. Lunar Science Conf. 6th, 2397–2415.Google Scholar
Gaffey, M. J. 1974, Ph.D. Thesis, MIT, Cambridge, Massachusetts.Google Scholar
Gault, D. G., and Heitowit, E. D. 1963, Proc. Sixth Hypervelocity Impact Symposium, vol. 2, pp. 419–456, Firestone Rubber Co., Cleveland, Ohio.Google Scholar
Levin, B. J. 1977, this book.Google Scholar
Morrison, D. 1977, this book.CrossRefGoogle Scholar
Stoffler, D., Gault, D. E., Wedekind, J., and Polkowski, G. 1975, J. Ceophys. Res., 80, 4062–4077.CrossRefGoogle Scholar
Zellner, B., Wisniewski, W.Z., Andersson, L., and Bowell, E. 1975, Astron. J., 80, 986–995.CrossRefGoogle Scholar
Zellner, B., and Gradie, J. 1976, Astron. J., 81, 262–280.CrossRefGoogle Scholar
Zellner, B., and Bowell, E. 1977, this book.Google Scholar