Core instability models of giant planet accretion and the planetary desert

dc.creatorMiguel, Yamila
dc.creatorBrunini, Adrian
dc.date.accessioned2018-05-07T11:53:30Z
dc.date.accessioned2018-11-06T14:41:14Z
dc.date.available2018-05-07T11:53:30Z
dc.date.available2018-11-06T14:41:14Z
dc.date.created2018-05-07T11:53:30Z
dc.date.issued2008-12
dc.identifierMiguel, Yamila; Brunini, Adrian; Core instability models of giant planet accretion and the planetary desert; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 387; 12-2008; 463-468
dc.identifier0035-8711
dc.identifierhttp://hdl.handle.net/11336/44259
dc.identifierCONICET Digital
dc.identifierCONICET
dc.identifier.urihttp://repositorioslatinoamericanos.uchile.cl/handle/2250/1889024
dc.description.abstractWith the aim of studying the final mass distribution of extrasolar planets, we have developed a simple model based on the core instability model, which allows us to form a large population of planets and make them evolve in circumstellar discs with various initial conditions. We investigate the consequences that different prescriptions for the solid and gas accretion rates would have on this distribution and found that it is strongly dependent on the adopted model for the gas accretion.
dc.languageeng
dc.publisherWiley Blackwell Publishing, Inc
dc.relationinfo:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1111/j.1365-2966.2008.13261.x
dc.relationinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/387/1/463/1002010
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.rightsinfo:eu-repo/semantics/openAccess
dc.subjectPlanets
dc.subjectSolar System formation
dc.subjectSatellites
dc.titleCore instability models of giant planet accretion and the planetary desert
dc.typeArtículos de revistas
dc.typeArtículos de revistas
dc.typeArtículos de revistas


Este ítem pertenece a la siguiente institución