The rotation rates of accreting planetesimals

Details The rotation rates of accreting planetesimals The rotation rates of accreting planetesimals

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982m%26p....26...89h&link_type=abstract

Moon and the Planets, vol. 26, Feb. 1982, p. 89-92.

Physics

1

Angular Velocity, Mass Distribution, Planetary Mass, Planetary Rotation, Protoplanets, Ceres Asteroid, Variable Mass Systems

Scientific paper

Analyses are presented of the rotation rates and relative rotation rates of accreting planetesimals. Specific attention is given to planetesimals of either constant or variable masses, and the mass distribution of the largest accreting planetesimal is assumed to be governed by a power law. An assumption of nearly constant mass during accretion is shown to be unrealistic, and an upper limit is derived to the relative velocity at infinity for a variable planetesimal mass. The formulations are applied to the asteroids Ceres and Pallas, and it is concluded that larger planets do not reach rotational instability by stochastic collisions during the final stages of accretion, while instability may be reached if relative velocities were greater than 2 km/sec during accumulation.

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