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Article: Planetary migration and eccentricity and inclination resonances in extrasolar planetary systems

TitlePlanetary migration and eccentricity and inclination resonances in extrasolar planetary systems
Authors
KeywordsCelestial mechanics
Planetary systems
Planets and satellites: general
Issue Date2009
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2009, v. 702 n. 2, p. 1662-1672 How to Cite?
AbstractThe differential migration of two planets due to planet-disk interaction can result in capture into the 2:1 eccentricity-type mean-motion resonances. Both the sequence of 2:1 eccentricity resonances that the system is driven through by continued migration and the possibility of a subsequent capture into the 4:2 inclination resonances are sensitive to the migration rate within the range expected for type II migration due to planet-disk interaction. If the migration rate is fast, the resonant pair can evolve into a family of 2:1 eccentricity resonances different from those found by Lee. This new family has outer orbital eccentricity e 2 ≳ 0.4-0.5, asymmetric librations of both eccentricity resonance variables, and orbits that intersect if they are exactly coplanar. Although this family exists for an inner-to-outer planet mass ratio m 1/m 2 ≳ 0.2, it is possible to evolve into this family by fast migration only for m 1/m 2 ≳ 2. Thommes and Lissauer have found that a capture into the 4:2 inclination resonances is possible only for m 1/m 2 ≲ 2. We show that this capture is also possible for m 1/m 2 ≳ 2 if the migration rate is slightly slower than that adopted by Thommes and Lissauer. There is significant theoretical uncertainty in both the sign and the magnitude of the net effect of planet-disk interaction on the orbital eccentricity of a planet. If the eccentricity is damped on a timescale comparable to or shorter than the migration timescale, e 2 may not be able to reach the values needed to enter either the new 2:1 eccentricity resonances or the 4:2 inclination resonances. Thus, if future observations of extrasolar planetary systems were to reveal certain combinations of mass ratio and resonant configuration, they would place a constraint on the strength of eccentricity damping during migration, as well as on the rate of the migration itself. © 2009 The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/129163
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
Funding AgencyGrant Number
NASANNG06GF42G
NSERC Canada
Funding Information:

It is a pleasure to thank Stan Peale for informative discussions. This research was supported in part by NASA grant NNG06GF42G (M. H. L.) and a grant from NSERC Canada (E. W. T.).

References

 

DC FieldValueLanguage
dc.contributor.authorLee, MHen_HK
dc.contributor.authorThommes, EWen_HK
dc.date.accessioned2010-12-23T08:33:12Z-
dc.date.available2010-12-23T08:33:12Z-
dc.date.issued2009en_HK
dc.identifier.citationAstrophysical Journal Letters, 2009, v. 702 n. 2, p. 1662-1672en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/129163-
dc.description.abstractThe differential migration of two planets due to planet-disk interaction can result in capture into the 2:1 eccentricity-type mean-motion resonances. Both the sequence of 2:1 eccentricity resonances that the system is driven through by continued migration and the possibility of a subsequent capture into the 4:2 inclination resonances are sensitive to the migration rate within the range expected for type II migration due to planet-disk interaction. If the migration rate is fast, the resonant pair can evolve into a family of 2:1 eccentricity resonances different from those found by Lee. This new family has outer orbital eccentricity e 2 ≳ 0.4-0.5, asymmetric librations of both eccentricity resonance variables, and orbits that intersect if they are exactly coplanar. Although this family exists for an inner-to-outer planet mass ratio m 1/m 2 ≳ 0.2, it is possible to evolve into this family by fast migration only for m 1/m 2 ≳ 2. Thommes and Lissauer have found that a capture into the 4:2 inclination resonances is possible only for m 1/m 2 ≲ 2. We show that this capture is also possible for m 1/m 2 ≳ 2 if the migration rate is slightly slower than that adopted by Thommes and Lissauer. There is significant theoretical uncertainty in both the sign and the magnitude of the net effect of planet-disk interaction on the orbital eccentricity of a planet. If the eccentricity is damped on a timescale comparable to or shorter than the migration timescale, e 2 may not be able to reach the values needed to enter either the new 2:1 eccentricity resonances or the 4:2 inclination resonances. Thus, if future observations of extrasolar planetary systems were to reveal certain combinations of mass ratio and resonant configuration, they would place a constraint on the strength of eccentricity damping during migration, as well as on the rate of the migration itself. © 2009 The American Astronomical Society. All rights reserved.en_HK
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.subjectCelestial mechanicsen_HK
dc.subjectPlanetary systemsen_HK
dc.subjectPlanets and satellites: generalen_HK
dc.titlePlanetary migration and eccentricity and inclination resonances in extrasolar planetary systemsen_HK
dc.typeArticleen_HK
dc.identifier.emailLee, MH:mhlee@hku.hken_HK
dc.identifier.authorityLee, MH=rp00724en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/0004-637X/702/2/1662en_HK
dc.identifier.scopuseid_2-s2.0-70549096168en_HK
dc.identifier.hkuros177708en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-70549096168&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume702en_HK
dc.identifier.issue2en_HK
dc.identifier.spage1662en_HK
dc.identifier.epage1672en_HK
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:000269245000069-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridLee, MH=7409119699en_HK
dc.identifier.scopusauthoridThommes, EW=6603411035en_HK

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