ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS
We study the orbital evolution of hot Jupiters due to the excitation and damping of tidally driven g-modes within solar-type host stars. Linearly resonant g-modes (the dynamical tide) are driven to such large amplitudes in the stellar core that they excite a sea of other g-modes through weakly nonli...
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| Format: | Article |
| Language: | en_US |
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IOP Publishing
2016
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| Online Access: | http://hdl.handle.net/1721.1/101660 https://orcid.org/0000-0001-9194-2084 https://orcid.org/0000-0001-8196-9267 |
| _version_ | 1826213322606772224 |
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| author | Weinberg, Nevin N. Essick, Reed Clasey |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Weinberg, Nevin N. Essick, Reed Clasey |
| author_sort | Weinberg, Nevin N. |
| collection | MIT |
| description | We study the orbital evolution of hot Jupiters due to the excitation and damping of tidally driven g-modes within solar-type host stars. Linearly resonant g-modes (the dynamical tide) are driven to such large amplitudes in the stellar core that they excite a sea of other g-modes through weakly nonlinear interactions. By solving the dynamics of large networks of nonlinearly coupled modes, we show that the nonlinear dissipation rate of the dynamical tide is several orders of magnitude larger than the linear dissipation rate. We find stellar tidal quality factors Q[' over *] ≃ 10[superscript 5]–10[superscript 6] for systems with planet mass M[subscript p] ≳ 0.5M[subscript J] and orbital period P ≲ 2\;\mathrm{days},$ which implies that such systems decay on timescales that are small compared to the main-sequence lifetime of their solar-type hosts. According to our results, there are ≃ 10 currently known exoplanetary systems, including WASP-19b and HAT-P-36-b, with orbital decay timescales shorter than a Gyr. Rapid, tidally induced orbital decay may explain the observed paucity of planets with M[subscript p] ≳ M[subscript J] and P < 2 days around solar-type hosts and could generate detectable transit-timing variations in the near future. |
| first_indexed | 2024-09-23T15:47:14Z |
| format | Article |
| id | mit-1721.1/101660 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T15:47:14Z |
| publishDate | 2016 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/1016602022-10-02T04:06:33Z ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS Weinberg, Nevin N. Essick, Reed Clasey Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Essick, Reed Clasey Weinberg, Nevin N. We study the orbital evolution of hot Jupiters due to the excitation and damping of tidally driven g-modes within solar-type host stars. Linearly resonant g-modes (the dynamical tide) are driven to such large amplitudes in the stellar core that they excite a sea of other g-modes through weakly nonlinear interactions. By solving the dynamics of large networks of nonlinearly coupled modes, we show that the nonlinear dissipation rate of the dynamical tide is several orders of magnitude larger than the linear dissipation rate. We find stellar tidal quality factors Q[' over *] ≃ 10[superscript 5]–10[superscript 6] for systems with planet mass M[subscript p] ≳ 0.5M[subscript J] and orbital period P ≲ 2\;\mathrm{days},$ which implies that such systems decay on timescales that are small compared to the main-sequence lifetime of their solar-type hosts. According to our results, there are ≃ 10 currently known exoplanetary systems, including WASP-19b and HAT-P-36-b, with orbital decay timescales shorter than a Gyr. Rapid, tidally induced orbital decay may explain the observed paucity of planets with M[subscript p] ≳ M[subscript J] and P < 2 days around solar-type hosts and could generate detectable transit-timing variations in the near future. National Science Foundation (U.S.) (Laser Interferometer Gravitational-Wave Observatory PHY-0757058) United States. National Aeronautics and Space Administration (NNX14AB40G) 2016-03-10T03:43:10Z 2016-03-10T03:43:10Z 2015-12 2015-08 Article http://purl.org/eprint/type/JournalArticle 1538-4357 0004-637X http://hdl.handle.net/1721.1/101660 Essick, Reed, and Nevin N. Weinberg. “ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS.” The Astrophysical Journal 816, no. 1 (December 23, 2015): 18. © 2016 The American Astronomical Society https://orcid.org/0000-0001-9194-2084 https://orcid.org/0000-0001-8196-9267 en_US http://dx.doi.org/10.3847/0004-637x/816/1/18 The Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf IOP Publishing IOP Publishing |
| spellingShingle | Weinberg, Nevin N. Essick, Reed Clasey ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS |
| title | ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS |
| title_full | ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS |
| title_fullStr | ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS |
| title_full_unstemmed | ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS |
| title_short | ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS |
| title_sort | orbital decay of hot jupiters due to nonlinear tidal dissipation within solar type hosts |
| url | http://hdl.handle.net/1721.1/101660 https://orcid.org/0000-0001-9194-2084 https://orcid.org/0000-0001-8196-9267 |
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