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The missing large impact craters on Ceres.

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Summary
This summary is machine-generated.

Ceres has far fewer large impact craters than expected, suggesting its surface has been resurfaced or its topography has relaxed over billions of years. This challenges asteroid impact models.

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Area of Science:

  • Planetary Science
  • Asteroid Science
  • Impact Cratering

Background:

  • Asteroids offer insights into planetesimal formation and evolution.
  • Collisional models predict numerous large craters (>400 km) on Ceres and Vesta based on asteroid belt depletion.
  • Ceres' surface shows a surprising lack of craters larger than ~280 km.

Purpose of the Study:

  • To investigate the discrepancy between predicted and observed impact craters on Ceres.
  • To reconcile observed cratering data with established collisional models for the asteroid belt.

Main Methods:

  • Analysis of cratering data on Ceres, focusing on sizes down to 100-150 km.
  • Comparison of observed crater populations with predictions from collisional models.
  • Consideration of alternative formation scenarios, including late implantation and resurfacing.

Main Results:

  • A significant depletion of craters on Ceres, even in the 100-150 km diameter range, was observed.
  • The scarcity of large craters contradicts predictions from standard collisional models.
  • This scarcity persists even when considering a late arrival of Ceres in the main asteroid belt.

Conclusions:

  • The observed cratering record on Ceres is incompatible with current collisional models.
  • A substantial number of large craters must have been erased on Ceres.
  • This obliteration implies either viscous relaxation of topography or extensive, long-term resurfacing processes on Ceres.