Direct Simulations of Growth from 1 km Planetesimals at 0.4 AU

Details Direct Simulations of Growth from 1 km Planetesimals at 0.4 AU Direct Simulations of Growth from 1 km Planetesimals at 0.4 AU

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dda....37.0303b&link_type=abstract

American Astronomical Society, DDA meeting #37, #3.03; Bulletin of the American Astronomical Society, Vol. 38, p.667

Astronomy and Astrophysics

Astronomy

Scientific paper

We present results of N-body simulations of planetesimal accretion beginning with 1 km-sized particles in orbit about a 1 solar mass star at 0.4 AU. Such particles may be the fundamental building blocks of terrestrial planets. This initial disk of planetesimals contains far too many bodies for any current N-body code to integrate, and we therefore only model a sample patch of the disk. Although this greatly reduces the number of bodies, our principal simulation still tracks over 100,000 particles in this manner. We consider several plausible initial conditions and monitor the growth of these particles. Our simulations use the perfect accretion model; planetesimal collisions are assumed to be completely inelastic. We integrate one patch for almost 1000 orbits and follow mass growth for over three orders of magnitude (the largest particle at the end of this simulation has a radius of over 12 km). Additionally, the escape speed of the largest particle grows considerably faster than the velocity dispersion of particles, suggesting impending runaway growth, although it is yet to begin in our simulations.

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