File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Diversity and origin of 2:1 Orbital resonances in extrasolar planetary systems

TitleDiversity and origin of 2:1 Orbital resonances in extrasolar planetary systems
Authors
KeywordsCelestial Mechanics
Planetary Systems
Planets And Satellites: General
Issue Date2004
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2004, v. 611 n. 1 I, p. 517-527 How to Cite?
AbstractA diversity of 2:1 resonance configurations can be expected in extrasolar planetary systems, and their geometry can provide information about the origin of the resonances. Assembly during planet formation by the differential migration of planets due to planet-disk interaction is one scenario for the origin of mean-motion resonances in extrasolar planetary systems. The stable 2:1 resonance configurations that can be reached by differential migration of planets with constant masses and initially coplanar and nearly circular orbits are (1) antisymmetric configurations with the mean-motion resonance variables θ1 = λ1 - 2λ2 + ω1 and θ2 = λ1 - 2λ2 + ω2 (where λj and ωj are the mean longitudes and the longitudes of periapse, respectively) librating about 0° and 180°, respectively (as in the Io-Europa pair), (2) symmetric configurations with both θ1 and θ2 librating about 0° (as in the GJ 876 system), and (3) asymmetric configurations with θ1 and θ2 librating about angles far from either 0° or 180°. There are, however, stable 2:1 resonance configurations with symmetric (θ1 ≈ θ2 ≈ 0°), asymmetric, and antisymmetric (θ1 ≈ 180° and θ2 ≈ 0°) librations that cannot be reached by differential migration of planets with constant masses and initially coplanar and nearly circular orbits. If real systems with these configurations are ever found, their origin would require (1) a change in the planetary mass ratio m1/m2 during migration, (2) a migration scenario involving inclination resonances, or (3) multiple-planet scattering in crowded planetary systems. We find that the asymmetric configurations with large e2 and the θ1 ≈ 180° and θ2 ≈ 0° configurations have intersecting orbits and that the θ1 ≈ θ2 ≈ 0° configurations with e1 > 0.714 have prograde periapse precessions.
Persistent Identifierhttp://hdl.handle.net/10722/151271
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorMan, HLen_US
dc.date.accessioned2012-06-26T06:19:47Z-
dc.date.available2012-06-26T06:19:47Z-
dc.date.issued2004en_US
dc.identifier.citationAstrophysical Journal Letters, 2004, v. 611 n. 1 I, p. 517-527en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/151271-
dc.description.abstractA diversity of 2:1 resonance configurations can be expected in extrasolar planetary systems, and their geometry can provide information about the origin of the resonances. Assembly during planet formation by the differential migration of planets due to planet-disk interaction is one scenario for the origin of mean-motion resonances in extrasolar planetary systems. The stable 2:1 resonance configurations that can be reached by differential migration of planets with constant masses and initially coplanar and nearly circular orbits are (1) antisymmetric configurations with the mean-motion resonance variables θ1 = λ1 - 2λ2 + ω1 and θ2 = λ1 - 2λ2 + ω2 (where λj and ωj are the mean longitudes and the longitudes of periapse, respectively) librating about 0° and 180°, respectively (as in the Io-Europa pair), (2) symmetric configurations with both θ1 and θ2 librating about 0° (as in the GJ 876 system), and (3) asymmetric configurations with θ1 and θ2 librating about angles far from either 0° or 180°. There are, however, stable 2:1 resonance configurations with symmetric (θ1 ≈ θ2 ≈ 0°), asymmetric, and antisymmetric (θ1 ≈ 180° and θ2 ≈ 0°) librations that cannot be reached by differential migration of planets with constant masses and initially coplanar and nearly circular orbits. If real systems with these configurations are ever found, their origin would require (1) a change in the planetary mass ratio m1/m2 during migration, (2) a migration scenario involving inclination resonances, or (3) multiple-planet scattering in crowded planetary systems. We find that the asymmetric configurations with large e2 and the θ1 ≈ 180° and θ2 ≈ 0° configurations have intersecting orbits and that the θ1 ≈ θ2 ≈ 0° configurations with e1 > 0.714 have prograde periapse precessions.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectCelestial Mechanicsen_US
dc.subjectPlanetary Systemsen_US
dc.subjectPlanets And Satellites: Generalen_US
dc.titleDiversity and origin of 2:1 Orbital resonances in extrasolar planetary systemsen_US
dc.typeArticleen_US
dc.identifier.emailMan, HL:mhlee@hku.hken_US
dc.identifier.authorityMan, HL=rp00724en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/422166en_US
dc.identifier.scopuseid_2-s2.0-5644273108en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-5644273108&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume611en_US
dc.identifier.issue1 Ien_US
dc.identifier.spage517en_US
dc.identifier.epage527en_US
dc.identifier.isiWOS:000223236000039-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridMan, HL=7409119699en_US

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats