Core instability models of giant planet accretion : II. Forming planetary systems

We develop a simple model for computing planetary formation based on the core instability model for the gas accretion and the oligarchic growth regime for the accretion of the solid core. In this model several planets can form simultaneously in the disc, a fact that has important implications especi...

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Detalles Bibliográficos
Autores principales: Miguel, Yamila, Brunini, Adrián
Formato: Articulo
Lenguaje:Inglés
Publicado: 2009
Materias:
Ciencias Astronómicas
planetología
astrofísica
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/2091
http://mnras.oxfordjournals.org/content/392/1/391
Aporte de:
Aportado por : SEDICI (UNLP) de Universidad Nacional de La Plata .
id I19-R120-10915-2091
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spelling I19-R120-10915-20912021-04-24T04:05:14Z http://sedici.unlp.edu.ar/handle/10915/2091 http://mnras.oxfordjournals.org/content/392/1/391 issn:1365-2966 Core instability models of giant planet accretion : II. Forming planetary systems Miguel, Yamila Brunini, Adrián 2009 2010-10-05T03:00:00Z en Ciencias Astronómicas planetología astrofísica We develop a simple model for computing planetary formation based on the core instability model for the gas accretion and the oligarchic growth regime for the accretion of the solid core. In this model several planets can form simultaneously in the disc, a fact that has important implications especially for the changes in the dynamic of the planetesimals and the growth of the cores since we consider the collision between them as a source of potential growth. The type I and type II migration of the embryos and the migration of the planetesimals due to the interaction with the disc of gas are also taken into account. With this model we consider different initial conditions to generate a variety of planetary systems and analyse them statistically. We explore the effects of using different type I migration rates on the final number of planets formed per planetary system such as on the distribution of masses and semimajor axis of extrasolar planets, where we also analyse the implications of considering different gas accretion rates. A particularly interesting result is the generation of a larger population of habitable planets when the gas accretion rate and type I migration are slower. Facultad de Ciencias Astronómicas y Geofísicas Articulo Articulo http://creativecommons.org/licenses/by-nc-nd/4.0/ Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0) application/pdf 391-399
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
planetología
astrofísica
spellingShingle Ciencias Astronómicas
planetología
astrofísica
Miguel, Yamila
Brunini, Adrián
Core instability models of giant planet accretion : II. Forming planetary systems
topic_facet Ciencias Astronómicas
planetología
astrofísica
description We develop a simple model for computing planetary formation based on the core instability model for the gas accretion and the oligarchic growth regime for the accretion of the solid core. In this model several planets can form simultaneously in the disc, a fact that has important implications especially for the changes in the dynamic of the planetesimals and the growth of the cores since we consider the collision between them as a source of potential growth. The type I and type II migration of the embryos and the migration of the planetesimals due to the interaction with the disc of gas are also taken into account. With this model we consider different initial conditions to generate a variety of planetary systems and analyse them statistically. We explore the effects of using different type I migration rates on the final number of planets formed per planetary system such as on the distribution of masses and semimajor axis of extrasolar planets, where we also analyse the implications of considering different gas accretion rates. A particularly interesting result is the generation of a larger population of habitable planets when the gas accretion rate and type I migration are slower.
format Articulo
Articulo
author Miguel, Yamila
Brunini, Adrián
author_facet Miguel, Yamila
Brunini, Adrián
author_sort Miguel, Yamila
title Core instability models of giant planet accretion : II. Forming planetary systems
title_short Core instability models of giant planet accretion : II. Forming planetary systems
title_full Core instability models of giant planet accretion : II. Forming planetary systems
title_fullStr Core instability models of giant planet accretion : II. Forming planetary systems
title_full_unstemmed Core instability models of giant planet accretion : II. Forming planetary systems
title_sort core instability models of giant planet accretion : ii. forming planetary systems
publishDate 2009
url http://sedici.unlp.edu.ar/handle/10915/2091
http://mnras.oxfordjournals.org/content/392/1/391
work_keys_str_mv AT miguelyamila coreinstabilitymodelsofgiantplanetaccretioniiformingplanetarysystems
AT bruniniadrian coreinstabilitymodelsofgiantplanetaccretioniiformingplanetarysystems
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