  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.
