Other
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm...p22b01i&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #P22B-01
Other
6022 Impact Phenomena, 6055 Surfaces And Interiors, 6205 Asteroids And Meteoroids
Scientific paper
A variety of explanations have been posited for the notable paucity of small craters on Eros. The spatial density of craters 200 m diameter and below decreases with decreasing diameter relative to an empirically saturated surface. Eros' surface exhibits a converse increase in boulder spatial density as well. Among the best explanations for the small crater depletion are: 1) the Yarkovsky effect; 2) the prevention of crater formation by impact into boulders; 3) and seismic shaking from other impacts. We have modeling of the latter process, starting with simple analytical models for seismic energy transmission of the surface and body waves induced by an impact event. Initial results show that craters as small as 100 m in diameter can be agents of surface alteration or resurfacing to one or more crater radii from the rim. These mechanisms can include: 1) launching loose surface materials on ballistic trajectories covering distances of centimeters to many meters; 2) inducing downslope movements; and 3) "sifting" of surface materials. Surface waves resulting from the formation of a crater of a given size can be effective at erasing or severely degrading craters of similar size or smaller up to several crater radii from the impact, and can affect lesser modifications of larger craters. Body waves are less effective over comparable distances through the interior of the asteroid. In the case of larger craters, however, both types of seismic waves may contribute effects across the entire asteroid. We will present analyses of seismic effects as possible causes of crater erasure and modification (e.g. mass wasting, "ponds" and "ghost craters").
Barnouin-Jha Olivier Serge
Izenberg Noam R.
Walch M. J.
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