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Timescales for planetary accretion and the structure of the protoplanetary diskModels 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.
Document ID
19870013947
Acquisition Source
Legacy CDMS
Document Type
Other
Authors
Lissauer, Jack J. (California Univ. Santa Barbara, CA, United States)
Date Acquired
September 5, 2013
Publication Date
May 1, 1987
Publication Information
Publication: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1986
Subject Category
Lunar And Planetary Exploration
Accession Number
87N23380
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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