Effect of the Seismic Shaking Erasure (revisited model) and Ejecta Coverage Erasure on the Crater Population of Asteroid 433 Eros

Details Effect of the Seismic Shaking Erasure (revisited model) and Ejecta Coverage Erasure on the Crater Population of Asteroid 433 Eros Effect of the Seismic Shaking Erasure (revisited model) and Ejecta Coverage Erasure on the Crater Population of Asteroid 433 Eros

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p51c1422b&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #P51C-1422

Physics

6017 Erosion And Weathering, 6022 Impact Phenomena (5420, 8136), 6055 Surfaces, 6205 Asteroids

Scientific paper

To explain the crater population of asteroid Eros, scenarios including impact-induced seismic shaking and ejecta coverage are proposed. The present study upgrades the erasure models considering the seismic shaking and the ejecta coverage processes. The ejecta coverage model, based on ballistic trajectory of ejecta blocks around an ellipsoidal model of asteroid Eros suggests a non negligible effect on the crater population of asteroid Eros. The seismic shaking model is improved by performing wave propagation simulation with the spectral-element method (Komatitsch and Tromp, 1999) applied to complex models of asteroid Eros, and a model of downslope movement has been developed. These simulations allow to compute the life time of a crater, corresponding to the time it will remain on the surface of Eros without being erased. These results are applied to different series of projectiles impacting Eros during different exposure times. This study highlights the importance of the regolith layer for trapping and amplifying seismic waves, like a wave guide. Also, we find a good agreement between the observed and the modeled crater population (including our erasure models) for an exposure time of 600 Myr. Finally, these results suggest an important contribution of the ejecta coverage process, as well as the seismic shaking erasure mechanism.

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