Fragmentation of colliding planetesimals with water content

Abstract

We investigate the outcome of collisions of Ceres-sized planetesimals composed of a rocky core and a shell of water ice. These collisions are not only relevant for explaining the formation of planetary embryos in early planetary systems, but also provide insight into the formation of asteroid families and possible water transport via colliding small bodies. Earlier studies show characteristic collision velocities exceeding the bodies' mutual escape velocity which - along with the distribution of the impact angles - cover the collision outcome regimes 'partial accretion', 'erosion', and 'hit-and-run' leading to different expected fragmentation scenarios. Existing collision simulations use bodies composed of strengthless material; we study the distribution of fragments and their water contents considering the full elasto-plastic continuum mechanics equations also including brittle failure and fragmentation.

arXiv commentSubmitted to IAU Symposium 310 Proceedings 4 pages, 2 figures

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• Asteroid flux towards circumprimary habitable zones in binary star systems: I. Statistical Overview
• The influence of orbital resonances on the water transport to objects in the circumprimary habitable zone of binary star systems
• Residual Neural Networks for the Prediction of Planetary Collision Outcomes
• The Formation of Habitable Planets in the Four-Planet System HD 141399
• On the formation of terrestrial planets between two massive planets: The case of 55 Cancri