Formation of the Giant Planets by Concurrant Accretion of Solids and Gas
摘要：
The actual rates at which the giant planets accreted small planetesimals is probably intermediate between the constant rates assumed in most previous studies and the highly variable rates used here. Within the context of the adopted model of planetesimal accretion, the joint constraints of the time scale for dissipation of the solar nebula and the current high- Z masses of the giant planets lead to estimates of the initial surface density (σ init ) of planetesimals in the outer region of the solar nebula. The results show that σ init ≈ 10 g cm 2 near Jupiter's orbit and that σ init ∝ a 2 , where a is the distance from the Sun. These values are a factor of 3 to 4 times as high as that of the "minimum-mass" solar nebula at Jupiter's distance and a factor of 2 to 3 times as high at Saturn's distance. The estimates for the formation time of Jupiter and Saturn are 1 to 10 million years, whereas those for Uranus fall in the range 2 to 16 million years. These estimates follow from the properties of our Solar System and do not necessarily apply to giant planets in other planetary systems.
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DOI：
10.1006/icar.1996.0190
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年份：
1995
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