Methods for computing giant planet formation and evolution
- Autores
- Benvenuto, Omar Gustavo; Brunini, Adrián
- Año de publicación
- 2005
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present a numerical code for computing all stages of the formation and evolution of giant planets in the framework of the core instability mechanism. This code is a non-trivial adaption of the stellar binary evolution code and is based on a standard Henyey technique. To investigate the performance of this code we applied it to the computation of the formation and evolution of a Jupiter mass object from a half Earth core mass to ages in excess of the age of the Universe. We also present a new smoothed linear interpolation algorithm devised especially for the purpose of circumventing some problems found when some physical data (e.g. opacities, equation of state, etc.) are introduced into an implicit algorithm like the one employed in this work.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Galaxies: evolution
Planets and satellites: formation - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/84285
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Methods for computing giant planet formation and evolutionBenvenuto, Omar GustavoBrunini, AdriánCiencias AstronómicasGalaxies: evolutionPlanets and satellites: formationWe present a numerical code for computing all stages of the formation and evolution of giant planets in the framework of the core instability mechanism. This code is a non-trivial adaption of the stellar binary evolution code and is based on a standard Henyey technique. To investigate the performance of this code we applied it to the computation of the formation and evolution of a Jupiter mass object from a half Earth core mass to ages in excess of the age of the Universe. We also present a new smoothed linear interpolation algorithm devised especially for the purpose of circumventing some problems found when some physical data (e.g. opacities, equation of state, etc.) are introduced into an implicit algorithm like the one employed in this work.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2005info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf1383-1395http://sedici.unlp.edu.ar/handle/10915/84285enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2004.08570.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:14Zoai:sedici.unlp.edu.ar:10915/84285Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:15.286SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
Methods for computing giant planet formation and evolution |
| title |
Methods for computing giant planet formation and evolution |
| spellingShingle |
Methods for computing giant planet formation and evolution Benvenuto, Omar Gustavo Ciencias Astronómicas Galaxies: evolution Planets and satellites: formation |
| title_short |
Methods for computing giant planet formation and evolution |
| title_full |
Methods for computing giant planet formation and evolution |
| title_fullStr |
Methods for computing giant planet formation and evolution |
| title_full_unstemmed |
Methods for computing giant planet formation and evolution |
| title_sort |
Methods for computing giant planet formation and evolution |
| dc.creator.none.fl_str_mv |
Benvenuto, Omar Gustavo Brunini, Adrián |
| author |
Benvenuto, Omar Gustavo |
| author_facet |
Benvenuto, Omar Gustavo Brunini, Adrián |
| author_role |
author |
| author2 |
Brunini, Adrián |
| author2_role |
author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas Galaxies: evolution Planets and satellites: formation |
| topic |
Ciencias Astronómicas Galaxies: evolution Planets and satellites: formation |
| dc.description.none.fl_txt_mv |
We present a numerical code for computing all stages of the formation and evolution of giant planets in the framework of the core instability mechanism. This code is a non-trivial adaption of the stellar binary evolution code and is based on a standard Henyey technique. To investigate the performance of this code we applied it to the computation of the formation and evolution of a Jupiter mass object from a half Earth core mass to ages in excess of the age of the Universe. We also present a new smoothed linear interpolation algorithm devised especially for the purpose of circumventing some problems found when some physical data (e.g. opacities, equation of state, etc.) are introduced into an implicit algorithm like the one employed in this work. Facultad de Ciencias Astronómicas y Geofísicas Instituto de Astrofísica de La Plata |
| description |
We present a numerical code for computing all stages of the formation and evolution of giant planets in the framework of the core instability mechanism. This code is a non-trivial adaption of the stellar binary evolution code and is based on a standard Henyey technique. To investigate the performance of this code we applied it to the computation of the formation and evolution of a Jupiter mass object from a half Earth core mass to ages in excess of the age of the Universe. We also present a new smoothed linear interpolation algorithm devised especially for the purpose of circumventing some problems found when some physical data (e.g. opacities, equation of state, etc.) are introduced into an implicit algorithm like the one employed in this work. |
| publishDate |
2005 |
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2005 |
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article |
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http://sedici.unlp.edu.ar/handle/10915/84285 |
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eng |
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