Giant Planet Formation, Evolution, and Internal Structure

Ravit Helled, Peter Bodenheimer, Morris Podolak, Aaron C. Boley, Farzana Meru, Sergei Nayakshin, Jonathan J. Fortney, Lucio Mayer, Yann Alibert, Alan P. Boss

Research output: Chapter in Book/Report/Conference proceedingChapterpeer-review


The large number of detected giant exoplanets offers the opportunity to improve our understanding of the formation mechanism, evolution, and interior structure of gas giant planets. The two main models for giant planet formation are core accretion and disk instability. There are substantial differences between these formation models, including formation timescale, favorable formation location, ideal disk properties for planetary formation, early evolution, planetary composition, etc. First, we summarize the two models including their substantial differences, advantages, and disadvantages, and suggest how theoretical models should be connected to available (and future) data. We next summarize current knowledge of the internal structures of solar — and extrasolar — giant planets. Finally, we suggest the next steps to be taken in giant planet exploration.
Original languageEnglish
Title of host publicationProtostars and planets VI
EditorsHenrik Beuther, Ralf S. Klessen, Cornelis P. Dullemond, Thomas Henning
Place of PublicationTucson, Arizona
PublisherTucson : University of Arizona Press
ISBN (Electronic)9780816598762
ISBN (Print)978-0-8165-3124-0
StatePublished - 2014

Publication series

NameThe University of Arizona space science series


  • Protostars -- Congresses
  • Planets -- Origin -- Congresses
  • Molecular clouds -- Congresses
  • Stars -- Formation -- Congresses


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