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Title:
Composition of massive giant planets
Authors:
Helled, Ravit; Bodenheimer, Peter; Lissauer, Jack J.
Affiliation:
AA(Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095-1567, USA ), AB(University of California, Santa Cruz, CA 95064, USA), AC(NASA-Ames Research Center, Moffett Field, CA 94035, USA)
Publication:
The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution, Proceedings of the International Astronomical Union, IAU Symposium, Volume 276, p. 95-100
Publication Date:
11/2011
Origin:
CUP
Keywords:
planets and satellites: formation, planetary systems: formation
Abstract Copyright:
(c) 2011: Copyright © International Astronomical Union 2011
DOI:
10.1017/S174392131102000X
Bibliographic Code:
2011IAUS..276...95H

Abstract

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.

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