The Stability of Protoplanet Systems

Details The Stability of Protoplanet Systems The Stability of Protoplanet Systems

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999icar..139..328y&link_type=abstract

Icarus, Volume 139, Issue Icarus, pp. 328-335.

Computer Science

26

Scientific paper

We investigated the stability of 10 protoplanet systems using three-dimensional N-body simulations. We found that the time scale of instability T depends strongly on the initial random velocities v (eccentricities e and inclinations i) and orbital separations Deltaa. For zero initial random velocities, we confirmed the result of Chambers et al. (1996, Icarus 119, 261-268) that T is proportional to exp(Deltaa). For finite random velocities, we found that T depends strongly on the initial random velocities. The relation between T and Deltaa is still expressed as logT=b+cDeltaa. However, both b and c depend on initial random velocities and the slope, b, becomes smaller for larger v. Even for relatively small initial eccentricities such as e~2r_H/a, where r_H is the Hill radius, the time scale can be reduced by a factor of 10 compared with the case of the zero random velocity. Therefore, the time scale of the formation of inner planets might be much shorter than what implied by Chambers et al.

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