Asteroidal regoliths

Details Asteroidal regoliths Asteroidal regoliths

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979icar...39..317h&link_type=abstract

Icarus, vol. 39, Sept. 1979, p. 317-351.

Astronomy and Astrophysics

Astronomy

45

Asteroids, Astronomical Models, Cratering, Planetary Evolution, Planetary Surfaces, Stony Meteorites, Infrared Imagery, Kinetic Energy, Meteorite Craters, Meteoritic Composition, Microwave Imagery, Planetary Structure, Radiation Effects, Velocity Distribution, Asteroids, Regolith, Models, Evolution, Depositional History, Ejecta, Cratering, Mixing, Fractionation, Depths, Data, Characteristics, Parent Bodies, Erosion, Blanketing, Parameters, High Strength Asteroids, Low Strength Asteroids, Polarization, Optic

Scientific paper

A physical model is developed for the evolution of regoliths on small bodies and applied to the asteroid and meteorite parent bodies. The model considers global deposition of that fraction of cratering ejecta that is not lost to space. In addition, it is applied to cases of both strong, cohesive bodies and to bodies of weak, unconsolidated materials. It is found that large, strong asteroids generate surficial regoliths of a few kilometers depth while strong asteroids smaller than 10-km diameter generate negligible regoliths. In conclusion, it is noted that the theory that substantial regoliths are produced predominantly by blanketing differs from earlier hypotheses that asteroidal regoliths might be thin or absent and that short surface exposure of asteroidal materials is due chiefly to erosion rather than blanketing.

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