On the mass distribution of planetesimals in the early runaway stage

Details On the mass distribution of planetesimals in the early runaway stage On the mass distribution of planetesimals in the early runaway stage

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998newa....3..411m&link_type=abstract

New Astronomy, vol. 3, no. 7, p. 411-416.

Astronomy and Astrophysics

Astronomy

25

Solar System: Formation, Planets And Satellites: General

Scientific paper

We derived the stationary distribution of the mass of planetesimals from the coagulation equation under the assumption of energy equipartition. In the three-dimensional case, we found that the stationary solution is expressed as n(m) ~ m^-8/3, where n is the surface number density and m is the mass of the planetesimals. This solution is in excellent agreement with the result of direct N-body simulations and the numerical integration of the coagulation equation, for the range of mass which contains most of the total mass of the planetesimals (10^22-10^25 g). In the two-dimensional case, the stationary solution exists but cannot be realized in a finite time. This difference is the direct consequence of the fact that runaway growth takes place in three dimensions, but not in two dimensions.

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