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Cited by 84Stellar, planetary, and galactic studiesAstro and Planetary ScienceHistory and Developments in Astronomy

TIDALLY DRIVEN ROCHE-LOBE OVERFLOW OF HOT JUPITERS WITH MESA

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Valsecchi, Francesca, Rappaport, Saul, Rasio, Frederic A., Marchant, Pablo, Rogers, Leslie A.·2015·The Astrophysical Journal
DOI 10.1088/0004-637x/813/2/101
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Abstract

Many exoplanets have now been detected in orbits with ultra-short periods very close to the Roche limit. Building upon our previous work, we study the possibility that mass loss through Roche lobe overflow (RLO) may affect the evolution of these planets, and could possibly transform a hot Jupiter into a lower-mass planet (hot Neptune or super-Earth). We focus here on systems in which the mass loss occurs slowly ("stable mass transfer" in the language of binary star evolution) and we compute their evolution in detail with the binary evolution code Modules for Experiments in Stellar Astrophysics. We include the effects of tides, RLO, irradiation, and photo-evaporation (PE) of the planet, as well as the stellar wind and magnetic braking. Our calculations all start with a hot Jupiter close to its Roche limit, in orbit around a Sun-like star. The initial orbital decay and onset of RLO are driven by tidal dissipation in the star. We confirm that such a system can indeed evolve to produce lower-mass planets in orbits of a few days. The RLO phase eventually ends and, depending on the details of the mass transfer and on the planetary core mass, the orbital period can remain around a few days for several Gyr. The remnant planets have rocky cores and some amount of envelope material, which is slowly removed via PE at a nearly constant orbital period; these have properties resembling many of the observed super-Earths and sub-Neptunes. For these remnant planets, we also predict an anti-correlation between mass and orbital period; very low-mass planets ( M pl ≲ 5 M ⊕ ) in ultra-short periods ( P orb < 1 day) cannot be produced through this type of evolution.

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  • Tidal mass loss can contribute to reversing a hot Jupiter's orbital decay.

    “This tidal mass loss can contribute to reversing a hot Jupiter's orbital decay (e.g., Valsecchi et al. 2015).”

    From Origins of Hot Jupiters (2018) · cites this paper as Valsecchi et al. 2015

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Cited by

Sorted by citations

Authors
Valsecchi, F., Rappaport, S., Rasio, F. A., Marchant, P., & Rogers, L. A.
Affiliations
  • Northwestern University (US)
  • Massachusetts Institute of Technology (US)
  • University of Bonn (DE)
  • California Institute of Technology (US)
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2015-11-03
Volume
813
Issue
2
Pages
101
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/813/2/101
OpenAlex
W3101280310
Cited by
84
References
2
Citations by year
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FWCI
5.31
Type
journal article
Language
en
Open access
Licence
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • Ghent University Academic Bibliography (Ghent University) (submittedVersion, cc-by)
  • CaltechAUTHORS (California Institute of Technology) (submittedVersion)
  • DSpace@MIT (Massachusetts Institute of Technology) (submittedVersion, cc-by-nc)
  • arXiv (Cornell University)
Funders
  • National Science Foundation (NAS 5-26555, 1126812)
  • National Aeronautics and Space Administration (NAS 526555, 526555, NNX12AI86G)
  • California Institute of Technology
  • Space Telescope Science Institute (NAS5- 26555, 5-26555, 26555)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › History and Developments in Astronomy
Keywords
hot Jupiters, Roche lobe overflow, planetary evolution, super-Earths, sub-Neptunes, tidal dissipation, stellar winds, magnetic braking, ultra-short-period planets, MESA

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