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Title:
On the Formation Timescale and Core Masses of Gas Giant Planets
Authors:
Rice, W. K. M.; Armitage, Philip J.
Affiliation:
AA(School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife KY16 9SS, UK ), AB(JILA, Campus Box 440, University of Colorado, Boulder CO 80309; Department of Astrophysical and Planetary Sciences, Campus Box 391, University of Colorado, Boulder CO 80309. )
Publication:
The Astrophysical Journal, Volume 598, Issue 1, pp. L55-L58. (ApJL Homepage)
Publication Date:
11/2003
Origin:
UCP
Astronomy Keywords:
Accretion, Accretion Disks, Stars: Planetary Systems: Formation, Planets and Satellites: Formation, Planets and Satellites: Individual: Jupiter, Solar System: Formation
DOI:
10.1086/380390
Bibliographic Code:
2003ApJ...598L..55R

Abstract

Numerical simulations show that the migration of growing planetary cores may be dominated by turbulent fluctuations in the protoplanetary disk, rather than by any mean property of the flow. We quantify the impact of this stochastic core migration on the formation timescale and core mass of giant planets at the onset of runaway gas accretion. For standard solar nebula conditions, the formation of Jupiter can be accelerated by almost an order of magnitude if the growing core executes a random walk with an amplitude of a few tenths of an AU. A modestly reduced surface density of planetesimals allows Jupiter to form within 10 Myr, with an initial core mass below 10 M, in better agreement with observational constraints. For extrasolar planetary systems, the results suggest that core accretion could form massive planets in disks with lower metallicities, and shorter lifetimes, than the solar nebula.
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