Composition of massive giant planets

Ravit Helled, Peter Bodenheimer, Jack J. Lissauer

Research output: Chapter in Book/Report/Conference proceedingConference contributionpeer-review

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.

Original languageEnglish
Title of host publicationThe Astrophysics of Planetary Systems
Subtitle of host publicationFormation, Structure, and Dynamical Evolution
EditorsAlessandro Sozzetti, Mario Lattanzi, Alan Boss
Pages95-100
Number of pages6
EditionS276
DOIs
StatePublished - Oct 2010
Externally publishedYes

Publication series

NameProceedings of the International Astronomical Union
NumberS276
Volume6
ISSN (Print)1743-9213
ISSN (Electronic)1743-9221

Keywords

  • Formation
  • Planetary systems
  • Planets and satellites

Fingerprint

Dive into the research topics of 'Composition of massive giant planets'. Together they form a unique fingerprint.

Cite this