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Erosive Hit-and-Run Impact Events: Debris Unbound

Published online by Cambridge University Press:  01 March 2016

Gal Sarid ,
Sarah T. Stewart  and
Zoë M. Leinhardt
Gal Sarid
Affiliation:
Florida Space Institute, University of Central Florida, Partnership 1 Building, 12354 Research Parkway, Suite 214, Orlando, FL, USA32826-0650 email: Gal.Sarid@ucf.edu
Sarah T. Stewart
Affiliation:
Department of Earth and Planetary Sciences, University of California Davis, One Shields Avenue, Davis, CAUSA95618 email: sts@ucdavis.edu
Zoë M. Leinhardt
Affiliation:
School of Physics, University of Bristol, H.H. Wills Physics Laboratory, Tyndall Avenue, Bristol, BS8 1TL, UK email: Zoe.Leinhardt@bristol.ac.uk
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Abstract

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Erosive collisions among planetary embryos in the inner solar system can lead to multiple remnant bodies, varied in mass, composition and residual velocity. Some of the smaller, unbound debris may become available to seed the main asteroid belt. The makeup of these collisionally produced bodies is different from the canonical chondritic composition, in terms of rock/iron ratio and may contain further shock-processed material. Having some of the material in the asteroid belt owe its origin from collisions of larger planetary bodies may help in explaining some of the diversity and oddities in composition of different asteroid groups.

Keywords

asteroidsminor planetssolar system: formationmethods: numerical

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