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The Astrophysical Journal, 613:L157L160, 2004 October 1 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A.
 

Summary: L157
The Astrophysical Journal, 613:L157L160, 2004 October 1
2004. The American Astronomical Society. All rights reserved. Printed in U.S.A.
ACCRETION EFFICIENCY DURING PLANETARY COLLISIONS
Craig Agnor and Erik Asphaug
Department of Earth Sciences, University of California at Santa Cruz, 1156 High Street, Santa Cruz, CA 95064; cagnor@es.ucsc.edu
Received 2004 March 29; accepted 2004 August 17; published 2004 August 31
ABSTRACT
We present the results of smoothed particle hydrodynamic simulations of collisions between two 0.10 M
differentiated planetary embryos with impact dynamics that are thought to be common to the late stage of
terrestrial planet formation. At low impact velocities ( ) and for direct collisions, the impacts arev /v ! 1.5imp esc
largely accretionary. Inelastic bouncing between embryos with varying degrees of erosion, followed by escape
to infinity, is also a common outcome. For dynamical environments typical of most late-stage accretion models,
we estimate that more than half of all collisions between like-sized planetary embryos do not result in accumulation
into a larger embryo.
Subject headings: accretion, accretion disks -- planets and satellites: formation -- solar system: formation
1. INTRODUCTION
The standard model for the formation of the terrestrialplanets
describes their growth as the collisional accumulation of rocky
planetesimals. This model is typically divided into three stages:

  

Source: Agnor, Craig B. - Astronomy Unit, School of Mathematical Sciences, Queen Mary, University of London

 

Collections: Physics