Timescales for planetary accretion and the structure of the protoplanetary disk

Details Timescales for planetary accretion and the structure of the protoplanetary disk Timescales for planetary accretion and the structure of the protoplanetary disk

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987icar...69..249l&link_type=abstract

Icarus (ISSN 0019-1035), vol. 69, Feb. 1987, p. 249-265.

Astronomy and Astrophysics

Astrophysics

288

Accretion Disks, Gas Giant Planets, Planetary Evolution, Planetary Structure, Protoplanets, Solar System, Asteroids, Jupiter (Planet), Solar Corona, Solar Orbits, Terrestrial Planets, Time Response, Planets, Time Scale, Accretion, Structure, Planetesimals, Solar System, Formation, Jupiter, Cores, Gases, Density, Mass, Models, Nebula, Mars, Gravity Effects, Orbits, Asteroids, Perturbations, Resonance, Viscosity, Escape, Ejection, Terrestrial Planets, Saturn, Neptune, Uranus, Comets, Angular Momentum, Calcula

Scientific paper

This paper outlines a unified scenario for Solar System formation consistent with astrophysical constraints. Jupiter's core could have grown by runaway accretion of planetesimals to a mass sufficient to initiate rapid accretion of gas in times of order of 5×105 - 106years. The inner planets and the asteroids can be accounted for if the surface density of the solar nebula was relatively uniform (decreasing no more rapidly than r-1/2) out to Jupiter's orbit. The total mass of the protoplanetary disk could have been less than one-tenth of a solar mass provided the surface density dropped off more steeply than r-1 beyond the orbit of Saturn. The outer regions of the nebula would still have contained enough solid matter to explain the growth of Uranus and Neptune in 5×106 - 108years, together with the coincident ejection of comets to the Oort cloud. The formation of such a protoplanetary disk requires significant transport of mass and angular momentum, and is consistent with viscous accretion disk models of the solar nebula.

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