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Article: Are the kepler near-resonance planet pairs due to tidal dissipation?
Title | Are the kepler near-resonance planet pairs due to tidal dissipation? |
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Authors | |
Keywords | Celestial mechanics Planetary systems Planets and satellites - general |
Issue Date | 2013 |
Publisher | The American Astronomical Society. The Journal's web site is located at http://iopscience.iop.org/0004-637X/ |
Citation | The Astrophysical Journal, 2013, v. 774, p. 52:1-52:8 How to Cite? |
Abstract | The multiple-planet systems discovered by the Kepler mission show an excess of planet pairs with period ratios just wide of exact commensurability for first-order resonances like 2:1 and 3:2. In principle, these planet pairs could have both resonance angles associated with the resonance librating if the orbital eccentricities are sufficiently small, because the width of first-order resonances diverges in the limit of vanishingly small eccentricity. We consider a widely held scenario in which pairs of planets were captured into first-order resonances by migration due to planet–disk interactions, and subsequently became detached from the resonances, due to tidal dissipation in the planets. In the context of this scenario, we find a constraint on the ratio of the planet’s tidal dissipation function and Love number that implies that some of the Kepler planets are likely solid. However, tides are not strong enough to move many of the planet pairs to the observed separations, suggesting that additional dissipative processes are at play. |
Persistent Identifier | http://hdl.handle.net/10722/189005 |
ISSN | 2023 Impact Factor: 4.8 2023 SCImago Journal Rankings: 1.905 |
ISI Accession Number ID |
DC Field | Value | Language |
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dc.contributor.author | Lee, MH | en_US |
dc.contributor.author | Fabrycky, D | en_US |
dc.contributor.author | Lin, DNC | en_US |
dc.date.accessioned | 2013-09-17T14:23:55Z | - |
dc.date.available | 2013-09-17T14:23:55Z | - |
dc.date.issued | 2013 | en_US |
dc.identifier.citation | The Astrophysical Journal, 2013, v. 774, p. 52:1-52:8 | en_US |
dc.identifier.issn | 0004-637X | - |
dc.identifier.uri | http://hdl.handle.net/10722/189005 | - |
dc.description.abstract | The multiple-planet systems discovered by the Kepler mission show an excess of planet pairs with period ratios just wide of exact commensurability for first-order resonances like 2:1 and 3:2. In principle, these planet pairs could have both resonance angles associated with the resonance librating if the orbital eccentricities are sufficiently small, because the width of first-order resonances diverges in the limit of vanishingly small eccentricity. We consider a widely held scenario in which pairs of planets were captured into first-order resonances by migration due to planet–disk interactions, and subsequently became detached from the resonances, due to tidal dissipation in the planets. In the context of this scenario, we find a constraint on the ratio of the planet’s tidal dissipation function and Love number that implies that some of the Kepler planets are likely solid. However, tides are not strong enough to move many of the planet pairs to the observed separations, suggesting that additional dissipative processes are at play. | - |
dc.language | eng | en_US |
dc.publisher | The American Astronomical Society. The Journal's web site is located at http://iopscience.iop.org/0004-637X/ | en_US |
dc.relation.ispartof | The Astrophysical Journal | en_US |
dc.subject | Celestial mechanics | - |
dc.subject | Planetary systems | - |
dc.subject | Planets and satellites - general | - |
dc.title | Are the kepler near-resonance planet pairs due to tidal dissipation? | en_US |
dc.type | Article | en_US |
dc.identifier.email | Lee, MH: mhlee@hku.hk | en_US |
dc.identifier.authority | Lee, MH=rp00724 | en_US |
dc.description.nature | published_or_final_version | - |
dc.identifier.doi | 10.1088/0004-637X/774/1/52 | - |
dc.identifier.scopus | eid_2-s2.0-84882771686 | - |
dc.identifier.hkuros | 222739 | en_US |
dc.identifier.volume | 774 | en_US |
dc.identifier.issue | 1 | - |
dc.identifier.spage | 52:1 | en_US |
dc.identifier.epage | 52:8 | en_US |
dc.identifier.eissn | 1538-4357 | - |
dc.identifier.isi | WOS:000323426700052 | - |
dc.publisher.place | United States | en_US |
dc.customcontrol.immutable | sml 140415 | - |
dc.identifier.issnl | 0004-637X | - |