CaltechAUTHORS
  A Caltech Library Service

Tidally-driven Roche-lobe Overflow of Hot Jupiters with MESA

Valsecchi, Francesca and Rappaport, Saul and Rasio, Frederic A. and Marchant, Pablo and Rogers, Leslie A. (2015) Tidally-driven Roche-lobe Overflow of Hot Jupiters with MESA. Astrophysical Journal, 813 (2). Art. No. 101. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20151222-095710796

[img] PDF - Published Version
See Usage Policy.

736Kb
[img] PDF - Submitted Version
See Usage Policy.

862Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20151222-095710796

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.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/813/2/101DOIArticle
http://iopscience.iop.org/article/10.1088/0004-637X/813/2/101/metaPublisherArticle
http://arxiv.org/abs/1506.05175arXivDiscussion Paper
ORCID:
AuthorORCID
Rogers, Leslie A.0000-0003-0638-3455
Additional Information:© 2015 The American Astronomical Society. Received 2015 June 16; accepted 2015 September 29; published 2015 November 3. WWe thank the anonymous referee for many very helpful comments. F.V. and F.A.R. are supported by NASA Grant NNX12AI86G. F.V. is also supported by a CIERA fellowship. L.A.R. gratefully acknowledges support provided by NASA through Hubble Fellowship grant #HF-51313 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. We thank Dorian Abbot, Arieh Konigl, Titos Matsakos, Ruth Murray-Clay, James Owen, and Dave Stevenson for useful discussions. This work used computing resources at CIERA funded by NSF PHY-1126812. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.
Funders:
Funding AgencyGrant Number
NASANNX12AI86G
Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)UNSPECIFIED
NASA Hubble FellowshipHF-51313
NASANAS 5-26555
NSFPHY-1126812
Subject Keywords:planet–star interactions – planetary systems – planets and satellites: gaseous planets – stars: evolution – stars: general
Record Number:CaltechAUTHORS:20151222-095710796
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20151222-095710796
Official Citation:Francesca Valsecchi et al 2015 ApJ 813 101
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:63132
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:22 Dec 2015 18:18
Last Modified:28 Aug 2017 22:08

Repository Staff Only: item control page