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Seismic resurfacing by a single impact on the asteroid 433 Eros


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 geology1,2. Asteroid 433 Eros, the most closely studied small body, has regions of substantially different crater densities3,4,5 that remain unexplained. Here we show that the formation of a relatively young crater (7.6 km in diameter) resulted in the removal of other craters as large as 0.5 km over nearly 40 per cent of the asteroid. Burial by ejecta cannot explain the observed pattern of crater removal. The limitation of reduced crater density to a zone within a particular straight-line distance through the asteroid from the centre of the large crater suggests degradation of the topography by seismic energy6 released during the impact. Our observations indicate that the interior of Eros is sufficiently cohesive to transmit seismic energy over many kilometres, and the outer several tens of metres of the asteroid must be composed of relatively non-cohesive material.

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Figure 1: Crater densities and other surface characteristics of Eros.
Figure 2: Transition between regions of different crater density.
Figure 3: Summary statistics of crater densities.


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This work was supported in part by the NASA Discovery Data Analysis Program. We are grateful to B. Carcich, to K. Consroe for technical help, and to M. Berthoud and J. Veverka for discussions. We also thank E. Asphaug and R. Greenberg.

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Thomas, P., Robinson, M. Seismic resurfacing by a single impact on the asteroid 433 Eros. Nature 436, 366–369 (2005).

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