Asteroidal agglutinate formation and implications for asteroidal surfaces

Details Asteroidal agglutinate formation and implications for asteroidal surfaces Asteroidal agglutinate formation and implications for asteroidal surfaces

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981icar...46..337h&link_type=abstract

Icarus, vol. 46, June 1981, p. 337-353.

Computer Science

45

Agglutination, Asteroids, Meteorites, Planetary Evolution, Craters, Ejecta, Glass, Impact Melts, Meteorite Collisions, Spallation, Asteroids, Surface, Agglutinates, Formation, Texture, Comparisons, Grains, Mineralogy, Petrology, Observations, Experiments, Energy, Impact Melts, Shock Heating, Cratering, Velocity, Models, Ejecta, Micrometeoroids, Collisions, Fragmentation, Spallation, Evolution

Scientific paper

The possible role of spallation on the free surfaces of target bodies in asteroid surface evolution in the presence of colliding bodies is considered. The ease of impact melt formation is discussed based on the results of shock recovery experiments, and a difference between collisions with dense, nonporous targets and with porous, particulate powders is demonstrated. It is shown that agglutinate-type glasses can be produced at impact velocities of 5 km/sec, but only in highly comminuted, porous targets and not in dense rocks. The apparent lack of agglutinate-type glasses on asteroid surfaces is explained in terms of coarse-grained asteroidal surfaces acting as dense, nonporous bedrock. It is argued that a possible mechanism inhibiting asteroidal surface comminution so as to inhibit melt formation and the effects of micrometeoroid impacts can be represented by collision processes with finite-sized targets rather than with a semi-infinite half-space as in the case of the moon, which give rise to spallation products rather than crater ejecta.

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