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Composition of massive giant planets

Published online by Cambridge University Press:  10 November 2011

Ravit Helled ,
Peter Bodenheimer  and
Jack J. Lissauer
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: rhelled@ucla.edu or r.helled@gmail.com
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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.

Keywords

planets and satellites: formationplanetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 95 - 100
Copyright
Copyright © International Astronomical Union 2011

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