Tidal Migration of Exoplanets around M Dwarfs: Frequency-dependent Tidal Dissipation
The orbital architectures of short-period exoplanet systems are shaped by tidal dissipation in their host stars. For low-mass M dwarfs whose dynamical tidal response comprises a dense spectrum of inertial modes at low frequencies, resolving the frequency dependence of tidal dissipation is crucial to...
| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad1e54 |
| _version_ | 1797293764279009280 |
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| author | Samantha C. Wu Janosz W. Dewberry Jim Fuller |
| author_facet | Samantha C. Wu Janosz W. Dewberry Jim Fuller |
| author_sort | Samantha C. Wu |
| collection | DOAJ |
| description | The orbital architectures of short-period exoplanet systems are shaped by tidal dissipation in their host stars. For low-mass M dwarfs whose dynamical tidal response comprises a dense spectrum of inertial modes at low frequencies, resolving the frequency dependence of tidal dissipation is crucial to capturing the effect of tides on planetary orbits throughout the evolutionary stages of the host star. We use nonperturbative spectral methods to calculate the normal mode oscillations of a fully convective M dwarf modeled using realistic stellar profiles from MESA. We compute the dissipative tidal response composed of contributions from each mode, as well as nonadiabatic coupling between the modes, which we find to be an essential component of the dissipative calculations. Using our results for dissipation, we then compute the evolution of circular, coplanar planetary orbits under the influence of tides in the host star. We find that orbital migration driven by resonance locking affects the orbits of Earth-mass planets at orbital periods P _orb ≲ 1.5 days and of Jupiter-mass planets at P _orb ≲ 2.5 days. Due to resonantly driven orbital decay and outward migration, we predict a dearth of small planets closer than P _orb ∼ 1 day and similarly sparse numbers of more massive planets out to P _orb ∼ 3 days. |
| first_indexed | 2024-03-07T21:20:35Z |
| format | Article |
| id | doaj.art-0a58313c544345a1a3a5ae3d051c63e5 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-07T21:20:35Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-0a58313c544345a1a3a5ae3d051c63e52024-02-27T13:26:12ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0196313410.3847/1538-4357/ad1e54Tidal Migration of Exoplanets around M Dwarfs: Frequency-dependent Tidal DissipationSamantha C. Wu0https://orcid.org/0000-0003-2872-5153Janosz W. Dewberry1https://orcid.org/0000-0001-9420-5194Jim Fuller2https://orcid.org/0000-0002-4544-0750California Institute of Technology , Astronomy Department, Pasadena, CA 91125, USA ; scwu@astro.caltech.edu; TAPIR, Mailcode 350-17, California Institute of Technology , Pasadena, CA 91125, USACITA , 60 St. George Street, Toronto, ON M5S 3H8, CanadaTAPIR, Mailcode 350-17, California Institute of Technology , Pasadena, CA 91125, USAThe orbital architectures of short-period exoplanet systems are shaped by tidal dissipation in their host stars. For low-mass M dwarfs whose dynamical tidal response comprises a dense spectrum of inertial modes at low frequencies, resolving the frequency dependence of tidal dissipation is crucial to capturing the effect of tides on planetary orbits throughout the evolutionary stages of the host star. We use nonperturbative spectral methods to calculate the normal mode oscillations of a fully convective M dwarf modeled using realistic stellar profiles from MESA. We compute the dissipative tidal response composed of contributions from each mode, as well as nonadiabatic coupling between the modes, which we find to be an essential component of the dissipative calculations. Using our results for dissipation, we then compute the evolution of circular, coplanar planetary orbits under the influence of tides in the host star. We find that orbital migration driven by resonance locking affects the orbits of Earth-mass planets at orbital periods P _orb ≲ 1.5 days and of Jupiter-mass planets at P _orb ≲ 2.5 days. Due to resonantly driven orbital decay and outward migration, we predict a dearth of small planets closer than P _orb ∼ 1 day and similarly sparse numbers of more massive planets out to P _orb ∼ 3 days.https://doi.org/10.3847/1538-4357/ad1e54Tidal interactionExoplanet tidesStar-planet interactions |
| spellingShingle | Samantha C. Wu Janosz W. Dewberry Jim Fuller Tidal Migration of Exoplanets around M Dwarfs: Frequency-dependent Tidal Dissipation The Astrophysical Journal Tidal interaction Exoplanet tides Star-planet interactions |
| title | Tidal Migration of Exoplanets around M Dwarfs: Frequency-dependent Tidal Dissipation |
| title_full | Tidal Migration of Exoplanets around M Dwarfs: Frequency-dependent Tidal Dissipation |
| title_fullStr | Tidal Migration of Exoplanets around M Dwarfs: Frequency-dependent Tidal Dissipation |
| title_full_unstemmed | Tidal Migration of Exoplanets around M Dwarfs: Frequency-dependent Tidal Dissipation |
| title_short | Tidal Migration of Exoplanets around M Dwarfs: Frequency-dependent Tidal Dissipation |
| title_sort | tidal migration of exoplanets around m dwarfs frequency dependent tidal dissipation |
| topic | Tidal interaction Exoplanet tides Star-planet interactions |
| url | https://doi.org/10.3847/1538-4357/ad1e54 |
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