Accretion of planetesimals within a gaseous ring

Details Accretion of planetesimals within a gaseous ring Accretion of planetesimals within a gaseous ring

Sep 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980aujph..33..623p&link_type=abstract

Australian Journal of Physics, vol. 33, Sept. 1980, p. 632-637.

Physics

9

Deposition, Equations Of Motion, Interplanetary Gas, Particle Motion, Planetary Evolution, Protoplanets, Angular Momentum, Coriolis Effect, Drag, Gas Density, Laplace Equation, Mars (Planet), Particle Spin, Particle Trajectories, Reynolds Number, Venus (Planet)

Scientific paper

The equations of motion of planetesimals accreted by a planetary embryo were examined by a modern Laplacian theory in the presence and absence of a gaseous torus centered on the same mean orbit. The torus gas density is assumed to be uniform and the drag on the particles was varied with the square of the relative velocity, correlating with the motion at a high Reynolds number. It was shown that the gas damps the Coriolis acceleration because of the presence of the sun in the rotating embryo, pulling the particles off the mean circular orbits and preventing accretion. At all times the accreting particles impart a spin angular momentum to the embryo; the actual spin rate decreases with greater gas drag, and is lowest for the innermost planets Mercury and Venus whose gas density is greatest.

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