Hostname: page-component-586b7cd67f-tf8b9 Total loading time: 0 Render date: 2024-11-25T21:43:18.523Z Has data issue: false hasContentIssue false

Physical Studies of Asteroids By Polarization of the Light

Published online by Cambridge University Press:  12 April 2016

Audouin Dollfus*
Affiliation:
Observatoire de Paris

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Curves of polarization are available at present for asteroids Vesta, Ceres, Pallas, Iris, Flora, and Icarus. These curves are compared with those of the satellites of Jupiter and Mercury, the Moon, and Mars. Laboratory simulations had already proved that the Moon's surface behaves like a powder of pulverized basalts; the recent confirmation by direct exploration is proving the significance of the method for remote determination of the surface properties of celestial bodies. The simulation of the Martian surface is found on small grained powders oxidized by ferreous limonite or goethite. New laboratory measurements were conducted to prepare the simulation of the asteroidal surfaces. Samples of the lunar surface returned to Earth provide impact-generated regolith and bare rocks superficially pitted and etched by impacts of the types suggested to be found on asteroidal surfaces; they were analyzed polarimetrically.

Preliminary interpretations show that Vesta departs significantly from the other asteroids and cannot be covered by frost deposits or by aggregate cosmic dusts; a regolith-type surface generated by impacts or a coating of cohesive grains is indicated.

Ceres, Pallas, and Iris are darker, and their polarizations do not suggest a pure regolithic surface, but cohesive grains or aggregates of dust are indicated.

Icarus is 108 times smaller in mass; its polarization authorizes a fluffy, loosely aggregated dust deposit; however, a cometary model with stones embedded in ice is perhaps not ruled out on the basis of the present data.

The way in which deep-space missions near the asteroidal belt can improve these results is discussed.

Type
Part I-Observations
Copyright
Copyright © NASA 1971

References

Dollfus, A. 1955, Étude des Planètes pai la Polarisation de la Lumière. Doctoral Thesis, Univ. of Paris. (1964, NASA TT F-188.)Google Scholar
Dollfus, A. 1956, Polarisation de la Lumière Renvoyée par les Corps Solides et les Nuages Naturels. Ann. Astrophys. 19, 83.Google Scholar
Dollfus, A. 1961, Polarization Studies of Planets. Planets and Satellites (ed., Kuiper, G.P.), pp. 389390. Univ. of Chicago Press. Chicago.Google Scholar
Dollfus, A. 1962, The Polarization of Moonlight. Physics and Astronomy of the Moon (ed., Kopal, Z.), ch. 5. Academic Press, Inc. London.Google Scholar
Dollfus, A., and Bowell, E. 1971, Polarimetrie Properties of the Lunar Surface and Its Interpretations, Part I. Telescopic Observations. Astron. Astrophys. 10, 2953.Google Scholar
Dollfus, A., Bowell, E., and Titulaer, C. 1971a, Polarimetrie Properties of the Lunar Surface and Its Interpretations, Part II. Terrestrial Samples in Orange Light. Astron. Astrophys. 10, 450466.Google Scholar
Dollfus, A., and Focas, J. 1969, La Planète Mars: La Nature de sa Surface et les Propriètés de son Atmosphere, d’Après la Polarisation de sa Lumière. I. Observations. Astron. Astrophys. 2, 6374.Google Scholar
Dollfus, A., Focas, J., and Bowell, E. 1969, La Planète Mars: La Nature de sa Surface et les Propriètés de son Atmosphere, d'Après la Polarisation de sa Lumière. II. La Nature du Sol de la Planète Mars. Astron. Astrophys. 2, 105121.Google Scholar
Dollfus, A., Geake, J., and Titulaer, C. 1971b, J. Geophys. Res., in press.Google Scholar
Dollfus, A., and Titulaer, C. 1971, Polarimetrie Properties of the Lunar Surface and Its Interpretation. Part III. Astron. Astrophys., in press.Google Scholar
Geake, J., Dollfus, A., Garlick, G., Lamb, W., Walker, G., Steigmann, G., and Titulaer, C. 1970, Luminescence, Electron Paramagnetic Resonance and Optical Properties of Lunar Material From Apollo 11. Proc. Apollo 11 Lunar Sci. Conf. Geochim. Cosmochim. Acta 34, suppl. 1, vol. 3, 21272147.Google Scholar
Gehrels, T., Roemer, E., Taylor, R., and Zellner, B. 1970, Minor Planets and Related Objects. IV. Asteroid (1566) Icarus. Astron. J. 75, 186195.Google Scholar
Lyot, B. 1929, Recherches sur la Polarisation de la Lumière des Planètes et de Quelques Substances Terrestres. Doctoral Thesis, Univ. of Paris. (1964, NASA TT F-187.)Google Scholar
Lyot, B. 1934, Polarisation des Petites Planètes. C.R. Acad. Sci. 199, 774.Google Scholar
McCord, B., Adams, J.B., and Johnson, T.V. 1970, Asteroid Vesta: Spectral Reflectivity and Compositional Implications. Science 168, 14451447.Google Scholar
Provin, S. 1955, Preliminary Observations of the Polarization of Asteioids. Publ. Astron. Soc. Pac. 67, 115.Google Scholar
Veverka, J. 1971, Photopolarimetric Observations of the Minoi Planet Flora. Icarus 15(3), in press.Google Scholar