Gas giant planets as dynamical barriers to inward-migrating super-Earths
| hal.structure.identifier | ECLIPSE 2015 | |
| dc.contributor.author | IZIDORO, A. | |
| hal.structure.identifier | ECLIPSE 2015 | |
| dc.contributor.author | RAYMOND, Sean N. | |
| hal.structure.identifier | Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides [CASSIOPEE] | |
| dc.contributor.author | MORBIDELLI, Alessandro, | |
| hal.structure.identifier | ECLIPSE 2015 | |
| dc.contributor.author | HERSANT, F. | |
| hal.structure.identifier | ECLIPSE 2015 | |
| dc.contributor.author | PIERENS, A. | |
| dc.date.issued | 2015 | |
| dc.identifier.issn | 2041-8205 | |
| dc.description.abstractEn | Planets of 1-4 times Earth's size on orbits shorter than 100 days exist around 30-50% of all Sun-like stars. In fact, the Solar System is particularly outstanding in its lack of "hot super-Earths" (or "mini-Neptunes"). These planets -- or their building blocks -- may have formed on wider orbits and migrated inward due to interactions with the gaseous protoplanetary disk. Here, we use a suite of dynamical simulations to show that gas giant planets act as barriers to the inward migration of super-Earths initially placed on more distant orbits. Jupiter's early formation may have prevented Uranus and Neptune (and perhaps Saturn's core) from becoming hot super-Earths. Our model predicts that the populations of hot super-Earth systems and Jupiter-like planets should be anti-correlated: gas giants (especially if they form early) should be rare in systems with many hot super-Earths. Testing this prediction will constitute a crucial assessment of the validity of the migration hypothesis for the origin of close-in super-Earths. | |
| dc.language.iso | en | |
| dc.publisher | Bristol : IOP Publishing | |
| dc.subject.en | Astrophysics - Earth and Planetary Astrophysics | |
| dc.title.en | Gas giant planets as dynamical barriers to inward-migrating super-Earths | |
| dc.type | Article de revue | |
| dc.identifier.doi | 10.1088/2041-8205/800/2/L22 | |
| dc.subject.hal | Physique [physics]/Astrophysique [astro-ph] | |
| dc.identifier.arxiv | 1501.06308 | |
| bordeaux.journal | The Astrophysical journal letters | |
| bordeaux.page | id. L22 | |
| bordeaux.volume | 800 | |
| bordeaux.issue | 2 | |
| bordeaux.peerReviewed | oui | |
| hal.identifier | hal-01110527 | |
| hal.version | 1 | |
| hal.popular | non | |
| hal.audience | Internationale | |
| hal.origin.link | https://hal.archives-ouvertes.fr//hal-01110527v1 | |
| bordeaux.COinS | ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=The%20Astrophysical%20journal%20letters&rft.date=2015&rft.volume=800&rft.issue=2&rft.spage=id.%20L22&rft.epage=id.%20L22&rft.eissn=2041-8205&rft.issn=2041-8205&rft.au=IZIDORO,%20A.&RAYMOND,%20Sean%20N.&MORBIDELLI,%20Alessandro,&HERSANT,%20F.&PIERENS,%20A.&rft.genre=article |
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