Growth model interpretation of planet size distribution
Li ZengCenter for Astrophysics | Harvard & Smithsonian, Department of Astronomy, Harvard University, MA 02138;S. B. JacobsenDepartment of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138;Dimitar SasselovCenter for Astrophysics | Harvard & Smithsonian, Department of Astronomy, Harvard University, MA 02138;M. I. PetaevCenter for Astrophysics | Harvard & Smithsonian, Department of Astronomy, Harvard University, MA 02138;Andrew VanderburgDepartment of Astronomy, The University of Texas at Austin, Austin, TX 78712;Mercedes López‐MoralesCenter for Astrophysics | Harvard & Smithsonian, Department of Astronomy, Harvard University, MA 02138;Juan Pérez‐MercaderDepartment of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138;Thomas R. MattssonHigh Energy Density Physics Theory Department, Sandia National Laboratories, Albuquerque, NM 87185;Gongjie LiSchool of Physics, Georgia Institute of Technology, Atlanta, GA 30313;Matthew Z. HeisingCenter for Astrophysics | Harvard & Smithsonian, Department of Astronomy, Harvard University, MA 02138;A. S. BonomoIstituto Nazionale di Astrofisica–Osservatorio Astrofisico di Torino, 10025 Pino Torinese, Italy;M. DamassoIstituto Nazionale di Astrofisica–Osservatorio Astrofisico di Torino, 10025 Pino Torinese, Italy;Travis A. BergerInstitute for Astronomy, University of Hawaii, Honolulu, HI 96822Hao CaoDepartment of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138;A. LeviCenter for Astrophysics | Harvard & Smithsonian, Department of Astronomy, Harvard University, MA 02138;Robin WordsworthDepartment of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138;
2019en
ABI
Аннотация
Significance The discovery of numerous exoplanet systems containing diverse populations of planets orbiting very close to their host stars challenges the planet formation theories based on the solar system. Here, we focus on the planets with radii of 2–4 R ⊕ , whose compositions are debated. They are thought to be either gas dwarfs consisting of rocky cores embedded in H 2 -rich gas envelopes or water worlds containing significant amounts of H 2 O-dominated fluid/ice in addition to rock and gas. We argue that these planets are water worlds.
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