36th DPS Meeting, 8-12 November 2004
Session 44 Origins and Planet Formation: Satellite Formation
Oral, Friday, November 12, 2004, 10:30am-12:00noon, Clark

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[44.05] The Growth of Terrestrial Planets: results from high resolution N-body simulations

Z.M. Leinhardt, D.C. Richardson (University of Maryland)

We will present the results of our most recent numerical simulations of terrestrial planet formation. We have developed the most realistic planetesimal collision model to date that handles accretion and erosion of planetesimals in a self-consistent manner. In our collision model gravity is the dominant mechanism in determining the collision outcome. We have fully integrated our collision model into a direct, parallelized, hierarchical, N-body code, called pkdgrav (Richardson et al. 2000, Stadel 2001) in order to study terrestrial planet formation in detail. We have run several numerical simulations with our collision model using similar initial conditions to previous numerical simulations (Kokubo and Ida 1998, 2000, 2002), allowing a straightforward basis for comparison. We have found that our "dust" component -- the particles that are below our resolution limit -- is potentially dynamically important, as suggested by Goldreich, Lithwick, and Sari (2004). We have also found that the general outcome of our simulations depends strongly on the initial conditions of the planetesimal disk and the collision model but is effectively independent of the coefficient of restitution of the planetesimals. In order to achieve higher resolution we will submit a large (106 particle) simulation to the Pittsburgh Supercomputer Center. This work is supported by the National Aeronautics and Space Administration under Grant Nos. NAG511722 and NGT550454 issued through the Office of Space Science.

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The author(s) of this abstract have provided an email address for comments about the abstract: zoe@astro.umd.edu

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Bulletin of the American Astronomical Society, 36 #4
© 2004. The American Astronomical Soceity.