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Composition of massive giant planets

Published online by Cambridge University Press:  10 November 2011

Ravit Helled
Affiliation:
Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095-1567, USA
Peter Bodenheimer
Affiliation:
University of California, Santa Cruz, CA 95064, USA
Jack J. Lissauer
Affiliation:
NASA-Ames Research Center, Moffett Field, CA 94035, USA email: [email protected] or [email protected]
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Abstract

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The two current models for giant planet formation are core accretion and disk instability. We discuss the core masses and overall planetary enrichment in heavy elements predicted by the two formation models, and show that both models could lead to a large range of final compositions. For example, both can form giant planets with nearly stellar compositions. However, low-mass giant planets, enriched in heavy elements compared to their host stars, are more easily explained by the core accretion model. The final structure of the planets, i.e., the distribution of heavy elements, is not firmly constrained in either formation model.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

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