Oligarchic planetesimal accretion and giant planet formation II

cic.isFulltexttruees
cic.isPeerReviewedtruees
cic.lugarDesarrolloUniversidad Nacional de La Plata es
cic.versioninfo:eu-repo/semantics/submittedVersiones
dc.date.accessioned2016-08-19T16:29:02Z
dc.date.available2016-08-19T16:29:02Z
dc.identifier.urihttps://digital.cic.gba.gob.ar/handle/11746/3868
dc.titleOligarchic planetesimal accretion and giant planet formation IIen
dc.typeComunicaciones
dcterms.abstractAims. The equation of state calculated by Saumon and collaborators has been adopted in most core-accretion simulations of giant-planet formation performed to date. Since some minor errors have been found in their original paper, we present revised simulations of giant-planet formation that considers a corrected equation of state. \nMethods. We employ the same code as Fortier and collaborators in repeating our previous simulations of the formation of Jupiter. \nResults. Although the general conclusions of Fortier and collaborators remain valid, we obtain significantly lower core masses and shorter formation times in all cases considered. \nConclusions. The minor errors in the previously published equation of state have been shown to affect directly the adiabatic gradient and the specific heat, causing an overestimation of both the core masses and formation times.en
dcterms.creator.authorFortier, Andreaes
dcterms.creator.authorBrunini, Adriánes
dcterms.creator.authorBenvenuto, Omar Gustavoes
dcterms.extentp. 1249-1252es
dcterms.identifier.other1432-0746es
dcterms.identifier.urlRecurso Completoes
dcterms.isPartOf.issuevol. 500, no. 3es
dcterms.isPartOf.seriesAstronomy and Astrophysicses
dcterms.issued2009-01-01
dcterms.languageEspañoles
dcterms.licenseAttribution 4.0 International (BY 4.0)es
dcterms.subjectplanetologíaes
dcterms.subject.materiaCiencias Astronómicases

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