The Evolution of the Solar Nebula with Nonuniform Viscosity and Planet Masses

Details The Evolution of the Solar Nebula with Nonuniform Viscosity and Planet Masses The Evolution of the Solar Nebula with Nonuniform Viscosity and Planet Masses

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...20517402j&link_type=abstract

American Astronomical Society Meeting 205, #174.02; Bulletin of the American Astronomical Society, Vol. 37, p.377

Astronomy and Astrophysics

Astronomy

2

Scientific paper

I investigate the surface density evolution of the solar nebula with nonuniform viscosity. The motivations are the following. 1) The author reported that nonuniform viscous frictional force in the solar nebula can account for the largest mass of Jupiter and Saturn and their largest amount of H and He among the planets and may have impact on planet masses; 2) Previous calculations of the nebula evolution have assumed uniform α viscosity and the current knowledge suggests that this may not be true; 3) The author showed that the nebula model of uniform α does not match the present planet mass distribution. The calculations are done by using currently accepted viscosity values and probable initial conditions from star formation theory. I find that the mass accumulation appears in Jupiter-Saturn region, which provides the mass supply for the formation of Jupiter and Saturn. The gas stays in the Jupiter-Saturn region long enough that they can capture large amount of gas, but not for Uranus and Neptune. Hence Jupiter and Saturn have larger masses with larger H and He content than Uranus and Neptune. I also study the impact on the masses of the terrestrial planets. Notice that the results here depend on the viscosity values, but not its details.

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