Evolution of random velocities of planetesimals in the course of accretion

Details Evolution of random velocities of planetesimals in the course of accretion Evolution of random velocities of planetesimals in the course of accretion

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992icar...98...20o&link_type=abstract

Icarus (ISSN 0019-1035), vol. 98, no. 1, July 1992, p. 20-27.

Physics

12

Gravitational Effects, Planetary Evolution, Protoplanets, Solar System Evolution, Kinetic Energy, Planetary Mass, Temperature Distribution

Scientific paper

The present examination of the role of accretion in planetesimals' random velocity evolution proceeds according to an equation for such evolution that is couched in terms of planetesimal orbits' eccentricity and inclination within the framework of Hill's approximations. The dissipation of random velocity by accretion leads to equipartition of the kinetic energy of random motion between planetesimals having different masses. At the earth's orbit, solar nebula gas drag, gravitational scattering, and accretion appear to contribute to the early stages of planetesimal accumulation's velocity evolution up to sizes of about 10 exp 20 g; they become less effective thereafter, and equilibrium velocities of planetesimals may then be determined by the interval between gravitational scattering and gas drag.

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