Numerical Integrations of the Accretion of Planetary Embryos

Details Numerical Integrations of the Accretion of Planetary Embryos Numerical Integrations of the Accretion of Planetary Embryos

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27..203c&link_type=abstract

Lunar and Planetary Science, volume 27, page 203

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Accretion: Planetary-Embryo, Dynamical Friction, N-Body Problem, Orbital Dynamics, Planets: Formation

Scientific paper

We present the results of long-term (up to 107-year) N-body integrations of systems of planetary embryos undergoing orbital and collisional evolution. The embryos represent the end products of the runaway growth stage of planet formation, and initially have widely-spaced non-crossing orbits. Long-range perturbations between embryos rapidly drive up the orbital eccentricities,e, until each object crosses the orbits of several neighbours and collisions between embryos occur. Perturbations continue to increase e, despite collisional damping, so that the system never returns to a state in which the embryos are isolated from one another. This behaviour remains essentially unchanged when up to 50% of the total mass is in the form of low-mass objects representing bodies that failed to be accreted by embryos during the runaway-growth stage.

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