Seismic resurfacing by a single impact on the asteroid 433 Eros

@article{Thomas2005SeismicRB,
  title={Seismic resurfacing by a single impact on the asteroid 433 Eros},
  author={Peter C. Thomas and Mark S. Robinson},
  journal={Nature},
  year={2005},
  volume={436},
  pages={366-369}
}
Impact cratering creates a wide range of topography on small satellites and asteroids. The population of visible craters evolves with impacts, and because there are no competing endogenic processes to modify the surface, determining the various ways younger craters add to or subtract from the population is a fundamental aspect of small-body geology. Asteroid 433 Eros, the most closely studied small body, has regions of substantially different crater densities that remain unexplained. Here we… 
Effects of ejecta accumulation on the crater population of asteroid 433 Eros
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References

SHOWING 1-10 OF 35 REFERENCES
The geology of 433 Eros
Abstract— The global high‐resolution imaging of asteroid 433 Eros by the Near‐Earth Asteroid Rendezvous (NEAR) Shoemaker spacecraft has made it possible to develop the first comprehensive picture of
Mechanical and geological effects of impact cratering on Ida
Asteroids respond to impact stresses differently from either laboratory specimens or large planets. Gravity is typically so small that seismic disturbances of a few cm s−1can devastate unconsolidated
Shoemaker crater as the source of most ejecta blocks on the asteroid 433 Eros
TLDR
It is suggested that most large ejecta blocks on Eros originate from a relatively young 7.6-km-diameter crater, and a large fraction of the ejecta from impacts pre-dating that crater has apparently been buried or eroded.
Impact-Induced Seismic Activity on Asteroid 433 Eros: A Surface Modification Process
TLDR
A combination of seismic and geomorphic modeling is used to analyze the response of regolith-covered topography, particularly craters, to impact-induced seismic shaking, and good agreement with the observed size-frequency distribution of craters is found, including the paucity of small craters.
Impact History of Eros: Craters and Boulders
Abstract Preliminary measurements of craters and boulders have been made in various locations on Eros from images acquired during the first nine months of NEAR Shoemaker's orbital mission, including
Compaction as the origin of the unusual craters on the asteroid Mathilde
The asteroid Mathilde has suffered at least five giant impacts. Previous studies suggest that Mathilde's giant craters should be surrounded by blankets of ejecta that are kilometres deep, yet the
Impacts on Asteroids: Fragmentation, Regolith Transport, and Disruption
Abstract We use a numerical hydrocode model to examine the outcomes of various size impacts into targets the sizes of Asteroids 951 Gaspra and 243 Ida, which were imaged by the Galileo spacecraft. A
Ejecta Emplacement on the Martian Satellites
Abstract Ejecta features on the martian satellites are compared to models of ballistic emplacement and downslope motion. The asymmetric distribution of ejecta around the large crater Stickney on
EROSION AND EJECTA REACCRETION ON 243 IDA AND ITS MOON
Abstract Galileo images of Asteroid 243 Ida and its satellite Dactyl show surfaces which are dominantly shaped by impact cratering. A number of observations suggest that ejecta from hypervelocity
Imaging of Small-Scale Features on 433 Eros from NEAR: Evidence for a Complex Regolith
TLDR
The subdued appearance of craters of different diameters and the variety of blocks and different degrees of their burial suggest that ejecta from several impact events blanketed the region imaged at closest approach and led to the building up of a substantial and complex regolith consisting of fine materials and abundant meter-sized blocks.
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