Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pggp.rept..100l&link_type=abstract
In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1986 p 100 (SEE N87-23341 16-91)
Astronomy and Astrophysics
Astrophysics
2
Accretion Disks, Astronomical Models, Astrophysics, Chronology, Protoplanets, Solar System, Angular Momentum, Mass Distribution, Mass Transfer, Nebulae, Star Formation
Scientific paper
Models of planetary accretion which assume the mass of condensable matter in the protoplanetary disk was equal to that present in the planets today predict accretion timescales for the outer planets approximately or less than 10 to the 8th years. Such timescales are inconsistent with observations of star forming regions, which suggest that most of the gas in disks around one solar mass is removed in a few x 10 to the 6th years. A unified scenario was outlined 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 500,000 to 5,000,000 years, provided the surface density of solids in its accretion zone was at least 5 to 10 times greater than that required by minimum mass models of the protoplanetary disk. The inner planets and the asteroids can be accounted for in this picture if the surface density of the solar nebula was relatively uniform out to Jupiter's orbit. 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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