• DOI:10.2458/azu_uapress_9780816531240-ch028
• Corpus ID: 118023784

Giant Planet Formation, Evolution, and Internal Structure

@article{Helled2014GiantPF,
  title={Giant Planet Formation, Evolution, and Internal Structure},
  author={Ravit Helled and Peter H. Bodenheimer and Morris Podolak and Aaron C. Boley and Farzana Meru and S Nayakshin and Jonathan J. Fortney and Lucio Mayer and Yann Alibert and Alan P. Boss},
  journal={arXiv: Earth and Planetary Astrophysics},
  year={2014},
  pages={643}
}

• R. Helled, P. Bodenheimer, +7 authors A. Boss
• Published 6 November 2013
• Geology, Physics
• arXiv: Earth and Planetary Astrophysics

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.