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dc.date.accessioned 2019-10-28T14:20:00Z
dc.date.available 2019-10-28T14:20:00Z
dc.date.issued 2011
dc.identifier.uri http://sedici.unlp.edu.ar/handle/10915/84176
dc.description.abstract Context.In the last few years, the so-called Nice model has become increasingly significant for studying the formation and evolution of the solar system. According to this model, the initial orbital configuration of the giant planets was much more compact than the one we observe today. Aims.We study the formation of the giant planets in connection with several parameters that describe the protoplanetary disk.We aim to establish which conditions enable their simultaneous formation in line with the initial configuration proposed by the Nice model. We focus on the conditions that lead to the simultaneous formation of two massive cores, corresponding to Jupiter and Saturn, which are able to reach the cross-over mass (where the mass of the envelope of the giant planet equals the mass of the core, and gaseous runway starts), while two other cores that correspond to Uranus and Neptune have to be able to grow to their current masses. Methods.We compute the in situ planetary formation, employing the numerical code introduced in our previous work for different density profiles of the protoplanetary disk. Planetesimal migration is taken into account and planetesimals are considered to follow a size distribution between rmin p (free parameter) and rmax p = 100 km. The core;s growth is computed according to the oligarchic growth regime. Results. The simultaneous formation of the giant planets was successfully completed for several initial conditions of the disk. We find that for protoplanetary disks characterized by a power law (r.p), flat surface density profiles (p . 1.5) favor the simultaneous formation. However, for steep slopes (p . 2, as previously proposed by other authors) the simultaneous formation of the solar system giant planets is unlikely. Conclusions. The simultaneous formation of the giant planets . in the context of the Nice model . is favored by flat surface density profiles. The formation time-scale agrees with the estimates of disk lifetimes if a significant mass of the solids accreted by the planets is contained in planetesimals with radii <1 km. en
dc.language en es
dc.subject methods: numerical es
dc.subject planet-disk interactions es
dc.subject planets and satellites: formation es
dc.title Simultaneous formation of solar system giant planets en
dc.type Articulo es
sedici.identifier.other doi:10.1051/0004-6361/201015731 es
sedici.identifier.other eid:2-s2.0-79961184131 es
sedici.identifier.issn 0004-6361 es
sedici.creator.person Guilera, Octavio Miguel es
sedici.creator.person Fortier, Andrea es
sedici.creator.person Brunini, Adrián es
sedici.creator.person Benvenuto, Omar Gustavo es
sedici.subject.materias Ciencias Astronómicas es
sedici.description.fulltext true es
mods.originInfo.place Facultad de Ciencias Astronómicas y Geofísicas es
mods.originInfo.place Instituto de Astrofísica de La Plata es
sedici.subtype Articulo es
sedici.rights.license Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
sedici.rights.uri http://creativecommons.org/licenses/by-nc-sa/4.0/
sedici.description.peerReview peer-review es
sedici.relation.journalTitle Astronomy and Astrophysics es
sedici.relation.journalVolumeAndIssue vol. 532 es
sedici.rights.sherpa * Color: verde* Pre-print del autor: si* Post-print del autor: si* Versión de editor/PDF:si* Condiciones:>>En el sitio web del autor o institucional o sitios que cumplan las directrices OAI>>Algunas revistas requieren un periodo de embargo para su depósito en repositorios recomendados por los organismos financiadores (ver revista)>>La versión de editor/PDF puede utilizarse (ver revista)>>Debe ir enlazado a la versión de editor>>Deben reconocerse el copyright y la fuente editorial>>No comercial* Link a Sherpa: http://sherpa.ac.uk/romeo/issn/0004-6361/es/


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Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) Except where otherwise noted, this item's license is described as Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)