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ICARUS 132, 113124 (1998) ARTICLE NO. IS985905

Summary: ICARUS 132, 113124 (1998)
N-Body Simulations of Late Stage Planetary Formation with a
Simple Fragmentation Model
S. G. Alexander
Physics Department, Miami University, Oxford, Ohio 45056
E-mail: alexansg@muohio.edu
C. B. Agnor
Physics Department, University of Colorado, Boulder, Colorado 80309
Received April 11, 1997; revised November 7, 1997
As the protoplanets undergo close encounters their
semi-major axes change substantially. This results in radialWe present results of two-dimensional gravitational N-body
simulations of the late stage of planetary formation. This stage mixing; thus, it is unlikely that the final planets grew in
is characterized by the direct accretion of hundreds of lunar- localized feeding zones. Instead, it is more likely that they
sized planetesimals into planetary bodies. Our simulation code formed from protoplanets which originated at a wide vari-
is based on the Hermite Individual Timestep integration algo- ety of radial distances (Wetherill 1994). Hence, any model-
rithm, and gravitational interactions among all bodies are in- ing of late stage planet formation must include protopla-
cluded throughout the simulations. We compare our simulation
nets that reflect this wide variety of initial semi-major axes


Source: Agnor, Craig B. - Astronomy Unit, School of Mathematical Sciences, Queen Mary, University of London
Alexander, Stephen G. - Department of Physics, Miami University (Ohio)


Collections: Physics