Orbital evolution of a circumbinary planet in a gaseous disk
Abstract Sub-Jupiter classed circumbinary planets discovered in close-in binary systems have orbits just beyond the dynamically unstable region, which is determined by the eccentricity and mass ratio of the host binary stars. These planets are assumed to have formed beyond the snow line and migrated...
| Main Authors: | , |
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| Format: | Article |
| Language: | English |
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SpringerOpen
2019-07-01
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| Series: | Earth, Planets and Space |
| Subjects: | |
| Online Access: | http://link.springer.com/article/10.1186/s40623-019-1064-0 |
| _version_ | 1828485292339757056 |
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| author | Akihiro Yamanaka Takanori Sasaki |
| author_facet | Akihiro Yamanaka Takanori Sasaki |
| author_sort | Akihiro Yamanaka |
| collection | DOAJ |
| description | Abstract Sub-Jupiter classed circumbinary planets discovered in close-in binary systems have orbits just beyond the dynamically unstable region, which is determined by the eccentricity and mass ratio of the host binary stars. These planets are assumed to have formed beyond the snow line and migrated to the current orbits rather than forming in situ. We propose a scenario in which a planet formed beyond the snow line and migrated to the inner edge of the circumbinary disk, which was within the unstable area, and then moved to the current orbit through outward transportation. This outward transportation is driven by the balance of orbital excitation of the central stars inside the gravitationally unstable region and damping by the gas-drag force. We carried out N-body simulations with a dissipating circumbinary protoplanetary disk for binary systems with different eccentricities and mass ratios. Planets are more likely to achieve a stable orbit just beyond the unstable region in less eccentric binary systems. This result is not as sensitive to mass ratio as it is to eccentricity. These dependencies are consistent with the data from observed binary systems hosting circumbinary planets. We find CBPs’ orbits close to the instability boundaries are explained by our orbital evolution scenario. |
| first_indexed | 2024-12-11T09:10:26Z |
| format | Article |
| id | doaj.art-a9c07ec13f1b4947b7e83f13c3f85c2e |
| institution | Directory Open Access Journal |
| issn | 1880-5981 |
| language | English |
| last_indexed | 2024-12-11T09:10:26Z |
| publishDate | 2019-07-01 |
| publisher | SpringerOpen |
| record_format | Article |
| series | Earth, Planets and Space |
| spelling | doaj.art-a9c07ec13f1b4947b7e83f13c3f85c2e2022-12-22T01:13:30ZengSpringerOpenEarth, Planets and Space1880-59812019-07-0171111210.1186/s40623-019-1064-0Orbital evolution of a circumbinary planet in a gaseous diskAkihiro Yamanaka0Takanori Sasaki1Department of Astronomy, Kyoto UniversityDepartment of Astronomy, Kyoto UniversityAbstract Sub-Jupiter classed circumbinary planets discovered in close-in binary systems have orbits just beyond the dynamically unstable region, which is determined by the eccentricity and mass ratio of the host binary stars. These planets are assumed to have formed beyond the snow line and migrated to the current orbits rather than forming in situ. We propose a scenario in which a planet formed beyond the snow line and migrated to the inner edge of the circumbinary disk, which was within the unstable area, and then moved to the current orbit through outward transportation. This outward transportation is driven by the balance of orbital excitation of the central stars inside the gravitationally unstable region and damping by the gas-drag force. We carried out N-body simulations with a dissipating circumbinary protoplanetary disk for binary systems with different eccentricities and mass ratios. Planets are more likely to achieve a stable orbit just beyond the unstable region in less eccentric binary systems. This result is not as sensitive to mass ratio as it is to eccentricity. These dependencies are consistent with the data from observed binary systems hosting circumbinary planets. We find CBPs’ orbits close to the instability boundaries are explained by our orbital evolution scenario.http://link.springer.com/article/10.1186/s40623-019-1064-0Planets and satellites: dynamical evolution and stabilityPlanets and satellites: formationPlanet–disk interactions |
| spellingShingle | Akihiro Yamanaka Takanori Sasaki Orbital evolution of a circumbinary planet in a gaseous disk Earth, Planets and Space Planets and satellites: dynamical evolution and stability Planets and satellites: formation Planet–disk interactions |
| title | Orbital evolution of a circumbinary planet in a gaseous disk |
| title_full | Orbital evolution of a circumbinary planet in a gaseous disk |
| title_fullStr | Orbital evolution of a circumbinary planet in a gaseous disk |
| title_full_unstemmed | Orbital evolution of a circumbinary planet in a gaseous disk |
| title_short | Orbital evolution of a circumbinary planet in a gaseous disk |
| title_sort | orbital evolution of a circumbinary planet in a gaseous disk |
| topic | Planets and satellites: dynamical evolution and stability Planets and satellites: formation Planet–disk interactions |
| url | http://link.springer.com/article/10.1186/s40623-019-1064-0 |
| work_keys_str_mv | AT akihiroyamanaka orbitalevolutionofacircumbinaryplanetinagaseousdisk AT takanorisasaki orbitalevolutionofacircumbinaryplanetinagaseousdisk |