New Formation Models for the Kepler-36 System

Bodenheimer, Peter; Stevenson, David J.; Lissauer, Jack J.; D’Angelo, Gennaro

doi:10.3847/1538-4357/aae928

Title: New Formation Models for the Kepler-36 System

Journal Article · Mon Dec 03 00:00:00 EST 2018 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aae928· OSTI ID:1511233

^[1];

^[2]; Lissauer, Jack J. ^[3];

^[4]

Univ. of California, Santa Cruz, CA (United States). UCO/Lick Observatory. Dept. of Astronomy and Astrophysics
California Inst. of Technology (CalTech), Pasadena, CA (United States). Division of Geological and Planetary Sciences
NASA Ames Research Center (ARC), Moffett Field, Mountain View, CA (United States). Space Science and Astrobiology Division
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)

Formation of the planets in the Kepler-36 system is modeled here by detailed numerical simulations according to the core-nucleated accretion scenario. The standard model is updated to include the dissolution of accreting rocky planetesimals in the gaseous envelope of the planet, leading to substantial enrichment of the envelope mass in heavy elements and a non-uniform composition with depth. For Kepler-36 c, models involving in situ formation and models involving orbital migration are considered. The results are compared with standard formation models. The calculations include the formation (accretion) phase as well as the subsequent cooling phase, up to the age of Kepler-36 (7 Gyr). During the latter phase, mass loss induced by stellar XUV radiation is included. In all cases, the results fit the measured mass, 7.84 M _⊕, and radius, 3.68 R _⊕, of Kepler-36 c. Two parameters are varied to obtain these fits: the disk solid surface density at the formation location and the "efficiency" factor in the XUV mass-loss rate. The updated models are hotter and therefore less dense in the silicate portion of the planet and in the overlying layers of H/He, as compared with standard models. The lower densities mean that only about half as much H/He is needed to be accreted to fit the present-day mass and radius constraints. For Kepler-36 b, an updated in situ calculation shows that the entire H/He envelope is lost, early in the cooling phase, in agreement with observation.

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Research Organization:: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States); NASA Ames Research Center (ARC), Moffett Field, Mountain View, CA (United States); Univ. of California, Santa Cruz, CA (United States); California Institute of Technology (CalTech), Pasadena, CA (United States)

Sponsoring Organization:: USDOE; National Aeronautics and Space Administration (NASA)

Grant/Contract Number:: 89233218CNA000001; 15-EW15_2-0007; NNX14AG92G

OSTI ID:: 1511233

Report Number(s):: LA-UR-18-23470

Journal Information:: The Astrophysical Journal (Online), Vol. 868, Issue 2; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 29 works

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