A reexamination of early numerical simulations of planetary accretion

Details A reexamination of early numerical simulations of planetary accretion A reexamination of early numerical simulations of planetary accretion

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pggp.rept..438k&link_type=abstract

In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990 p 438-440 (SEE N92-10728 01-91)

Physics

Geophysics

Algorithms, Astronomical Models, Computerized Simulation, Planetary Evolution, Protoplanets, Collisions, Continuums, Size Distribution, Stellar Mass Accretion, Velocity Distribution

Scientific paper

The intermediate stage of protoplanetary accretion, where sub-km sized bodies accrete in 500-1000 km diameter bodies, is critical in determining the character of subsequent evolution. Greenberg et al. discovered that, at least through the formation of 500 km planetary embryos, the small particle dominate the population and control the velocity distribution, keeping velocities much smaller and setting up the possibility of runaway accretion, where the largest body is able to accumulate quickly a much greater mass and separate itself from the continuum of the size distribution. However, some controversy remains as to the exact methods used by Greenberg et al. I reviewed that planet formation model in detail to address these criticisms and better explain the algorithm used in the study. In particular, the algorithms for mutual velocity stirring among planetesimals and mass shifting between adjacent diameter bins are rederived in detail. I also examined the likelihood of artificial acceleration of the runaway growth phase of the intermediate stage of planetesimal formation.

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