Analysis of the kinematics of ejecta created after a catastrophic collision

Journal
Date Issued
2015
Author(s)
•
•
Paolicchi, P.
•
Tanga, P.
DOI
Description
Acknowledgments The authors are grateful to two anonymous reviewers for their constructive comments.
Abstract
According to the results of hydrodynamical simulations, the creation of an asteroid dynamical family as the outcome of a high-energy collision consists of the partial or complete shattering of the parent body followed by re-accumulation of many fragments into larger bodies due to the mutual gravity. This scenario seems to reproduce satisfactorily the observed properties of the asteroid families, and in particular the size distribution of the members. In this paper we show a preliminary analysis of the ejection velocity fields predicted by hydrodynamical models, in comparison with the ejection velocity fields simulated by semi-empirical models, in order to identify the features of the velocity distribution that trigger or prevent the fragments' gravitational re-accumulation.

Volume
118
Start page
285
Uri
Url
Issn Identifier
0032-0633
Ads BibCode
2015P&SS..118..285D
Rights
open.access
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