Three regimes of extrasolar planet radius inferred from host star metallicities

Lars A. Buchhave (), Martin Bizzarro, David W. Latham, Dimitar Sasselov, William D. Cochran, Michael Endl, Howard Isaacson, Diana Juncher and Geoffrey W. Marcy
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Lars A. Buchhave: Harvard-Smithsonian Center for Astrophysics
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
Geoffrey W. Marcy: University of California

Nature, 2014, vol. 509, issue 7502, 593-595

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.

Date: 2014
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DOI: 10.1038/nature13254

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