Mostrar el registro sencillo del ítem

Planet-planet scattering in planetesimal disks II: Predictions for outer extrasolar planetary systems

hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
dc.contributor.authorRAYMOND, Sean N.
dc.contributor.authorARMITAGE, Philip J.
dc.contributor.authorGORELICK, Noel
dc.date.created2010-01-20
dc.date.issued2010
dc.identifier.issn0004-637X
dc.description.abstractEnWe develop an idealized dynamical model to predict the typical properties of outer extrasolar planetary systems, at radii beyond 5 AU. Our hypothesis is that dynamical evolution in outer planetary systems is controlled by a combination of planet-planet scattering and planetary interactions with an exterior disk of small bodies ("planetesimals"). Using 5,000 long duration N-body simulations, we follow the evolution of three planets surrounded by a 50 Earth mass primordial planetesimal disk. For large planet masses (above that of Saturn) the influence of the disk is modest, and we recover the observed eccentricity distribution of extrasolar planets (observed primarily at smaller radii). We explain the observed mass dependence of the eccentricity by invoking strong correlations between planet masses in the same system. For lower mass planets we observe diverse dynamical behavior: strong scattering events, sudden jumps in eccentricity due to resonance crossings, and re-circularization of scattered low-mass planets in the disk. We present distributions of the final eccentricity and inclination, and discuss how they vary with planet mass and initial system architecture. We predict a transition to lower eccentricities for low mass planets at radii where disks influence the dynamics. Radial velocity measurements capable of detecting planets with K~5 m/s and periods in excess of 10 years will constrain this regime. We also study the population of resonant and non-resonant multiple planet systems. We show that, among systems with Jupiter-mass planets that avoid close encounters, the planetesimal disk acts as a damping mechanism that frequently populates mean motion resonances. Resonant chains ought to be common among massive planets in outer planetary systems.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.encelestial mechanics
dc.subject.enplanet-disk interactions
dc.subject.enplanetary systems
dc.subject.enplanets and satellites: dynamical evolution and stability
dc.subject.enplanets and satellites: formation
dc.title.enPlanet-planet scattering in planetesimal disks II: Predictions for outer extrasolar planetary systems
dc.typeArticle de revue
dc.identifier.doi10.1088/0004-637X/711/2/772
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1001.3409
bordeaux.journalThe Astrophysical Journal
bordeaux.page772-795
bordeaux.volume711
bordeaux.issue2
bordeaux.peerReviewedoui
hal.identifierhal-00473128
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00473128v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=The%20Astrophysical%20Journal&rft.date=2010&rft.volume=711&rft.issue=2&rft.spage=772-795&rft.epage=772-795&rft.eissn=0004-637X&rft.issn=0004-637X&rft.au=RAYMOND,%20Sean%20N.&ARMITAGE,%20Philip%20J.&GORELICK,%20Noel&rft.genre=article


Archivos en el ítem

ArchivosTamañoFormatoVer

No hay archivos asociados a este ítem.

Este ítem aparece en la(s) siguiente(s) colección(ones)

Mostrar el registro sencillo del ítem