Afficher la notice abrégée

hal.structure.identifierDepartment of Archaeology
dc.contributor.authorWALSH, K. J.
hal.structure.identifierLaboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides [CASSIOPEE]
dc.contributor.authorMORBIDELLI, A.
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierUniversité Sciences et Technologies - Bordeaux 1 [UB]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
dc.contributor.authorRAYMOND, Sean N.
dc.contributor.authorO'BRIEN, D. P.
dc.contributor.authorMANDELL, A. M.
dc.date.conference2010
dc.description.abstractEnNumerical simulations of planetary accretion have succeeded in matching most of the physical and orbital properties of the terrestrial planets with one glaring exception: they categorically form Mars analogs that are roughly an order of magnitude too massive (Raymond et al. 2009). The initial conditions that best reproduce the mass of Mars require that the inner planetesimal disk had an outer edge at 1 Astronomical Unit (AU) (Hansen 2009). To date, no mechanism has been shown to create this edge and remain compatible with the current-day solar system, in particular the existence of the asteroid belt. Here we show that a substantial gas-driven radial migration of the giant planets is the needed mechanism. Hydrodynamical simulations show that the evolution of Jupiter and Saturn in a gas-disk generically leads to a two-stage, inward-then-outward, migration where the extent of each stage of migration depends on a priori unconstrained disk parameters (Masset & Snellgrove 2001, Morbidelli et al. 2007, Pierens & Nelson 2008). We demonstrate with numerical simulations that, if Jupiter migrated inwards to 1.5 AU before migrating out towards its current location, its gravitational influence would truncate the inner planetesimal disk at 1 AU. The resulting disk naturally reproduces all the terrestrial planets including Mars. During the giant planets' migration, the asteroid belt is emptied and later re-populated from two distinct parent populations. This provides the first dynamical explanation for the current dichotomy of physical properties of the main asteroid belt, with anhydrous asteroids (S-type) in the inner part and primitive asteroids (C-type) in the outer part (Gradie & Tedesco 1982). Our model links the origin of the inner solar system -- explaining the mass of Mars and the properties of the asteroid belt -- to a realistic evolution of the giant planets. Thus Mars and the asteroid belt provide the first evidence for an early solar system evolution characterized by substantial gas-driven orbital migration of the giant planets, similar to what is inferred for extrasolar planet systems (Armitage 2007).
dc.language.isoen
dc.subject.en[5205] PLANETARY SCIENCES: ASTROBIOLOGY
dc.subject.enFormation of stars and planets
dc.subject.en[5225] PLANETARY SCIENCES: ASTROBIOLOGY
dc.subject.enEarly environment of Earth
dc.subject.en[5455] PLANETARY SCIENCES: SOLID SURFACE PLANETS
dc.subject.enOrigin and evolution
dc.title.enThe Low Mass of Mars: First Evidence of Early Gas-Driven Migration by Jupiter
dc.typeCommunication dans un congrès
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]
bordeaux.conference.titleAmerican Geophysical Union, Fall Meeting 2010, abstract #V53A-2233
bordeaux.countryUS
bordeaux.peerReviewedoui
hal.identifierhal-00582367
hal.version1
hal.invitednon
hal.proceedingsnon
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00582367v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.au=WALSH,%20K.%20J.&MORBIDELLI,%20A.&RAYMOND,%20Sean%20N.&O'BRIEN,%20D.%20P.&MANDELL,%20A.%20M.&rft.genre=unknown


Fichier(s) constituant ce document

FichiersTailleFormatVue

Il n'y a pas de fichiers associés à ce document.

Ce document figure dans la(les) collection(s) suivante(s)

Afficher la notice abrégée