Are carbonaceous chondrites coming from the outer Solar System?

PARISI, M. G.; SANTAMARÍA, P.; DI SISTO, R.; DE ELIA, G.

Cordoba

Taller; VII Taller de Ciencias Planetarias; 2014

Observatorio Astronomico de Cordoba

PRE.cjk { font-family: "Droid Sans",monospace; }PRE.ctl { font-family: "FreeSans",monospace; }P { margin-bottom: 0.21cm; } Parisi(2013) has shown that a dynamically cold disk would be required for the formation and evolution of planetesimals of different sizes during all the planetary formation process at all locations in the disk. This is consistent with recent laboratory experiments where it was shown that the internal structure of carbonaceous chondrites implies that their parent objects had never collided at a speed higher than around 200-400 m/s (Beitz et al.2013). Motivated by these results, we investigate a new possible scenario for the source of carbonaceous chondrites looking for low velocity collisions among carbonaceous chondrites parent bodies candidates in the Kuiper Belt within the framework of the Nice Model.