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Science 20 June 1997:
Vol. 276. no. 5320, pp. 1836 - 1839
DOI: 10.1126/science.276.5320.1836
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Reports

Giant Planet Formation by Gravitational Instability

Alan P. Boss

The recent discoveries of extrasolar giant planets, coupled with refined models of the compositions of Jupiter and Saturn, prompt a reexamination of theories of giant planet formation. An alternative to the favored core accretion hypothesis is examined here; gravitational instability in the outer solar nebula leading to giant planet formation. Three-dimensional hydrodynamic calculations of protoplanetary disks show that giant gaseous protoplanets can form with locally isothermal or adiabatic disk thermodynamics. Gravitational instability appears to be capable of forming giant planets with modest cores of ice and rock faster than the core accretion mechanism can.

Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015-1305, USA.

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THIS ARTICLE HAS BEEN CITED BY OTHER ARTICLES:
Direct Imaging of Multiple Planets Orbiting the Star HR 8799.
C. Marois, B. Macintosh, T. Barman, B. Zuckerman, I. Song, J. Patience, D. Lafreniere, and R. Doyon (2008)
Science 322, 1348-1352
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Formation of Giant Planets by Fragmentation of Protoplanetary Disks.
L. Mayer, T. Quinn, J. Wadsley, and J. Stadel (2002)
Science 298, 1756-1759
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Discovery of Young, Isolated Planetary Mass Objects in the sigma Orionis Star Cluster.
M. R. Zapatero Osorio, V. J. S. Béjar, E. L. Martín, R. Rebolo, D. B. y Navascués, C. A. L. Bailer-Jones, and R. Mundt (2000)
Science 290, 103-107
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Evidence for Dust Grain Growth in Young Circumstellar Disks.
H. B. Throop, J. Bally, L. W. Esposito, and M. J. McCaughrean (2001)
Science 292, 1686-1689
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