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Three regimes of extrasolar planet radius inferred from host star metallicities

Author

Listed:
  • Lars A. Buchhave

    (Harvard-Smithsonian Center for Astrophysics
    Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark)

  • Martin Bizzarro

    (Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark)

  • David W. Latham

    (Harvard-Smithsonian Center for Astrophysics)

  • Dimitar Sasselov

    (Harvard-Smithsonian Center for Astrophysics)

  • William D. Cochran

    (McDonald Observatory, The University of Texas)

  • Michael Endl

    (McDonald Observatory, The University of Texas)

  • Howard Isaacson

    (University of California)

  • Diana Juncher

    (Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark
    Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark)

  • Geoffrey W. Marcy

    (University of California)

Abstract

Analysis of the metallicities of more than 400 stars hosting 600 candidate extrasolar planets shows that the planets can be categorized by size into three populations — terrestrial-like planets, gas dwarf planets with rocky cores and hydrogen–helium envelopes, and ice or gas giant planets — on the basis of host star metallicity.

Suggested Citation

  • Lars A. Buchhave & Martin Bizzarro & David W. Latham & Dimitar Sasselov & William D. Cochran & Michael Endl & Howard Isaacson & Diana Juncher & Geoffrey W. Marcy, 2014. "Three regimes of extrasolar planet radius inferred from host star metallicities," Nature, Nature, vol. 509(7502), pages 593-595, May.
    • Handle: RePEc:nat:nature:v:509:y:2014:i:7502:d:10.1038_nature13254
    DOI: 10.1038/nature13254
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