Terrestrial-type planet formation. Comparing different types of initial conditions
- Autores
- Ronco, María Paula; de Elia, Gonzalo Carlos; Guilera, Octavio Miguel
- Año de publicación
- 2015
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. The initial distributions of planetary embryos and planetesimals used in N-body simulations play an important role for studies of the terrestrial-type planet formation during the post oligarchic growth. In general, most of these studies typically use ad hoc initial distributions based primarily on theoretical and numerical studies. Aims. We analyze the formation of planetary systems without gas giants around solar-type stars by focusing on the sensitivity of the results to the particular initial distributions used for planetesimals and planetary embryos at the end of the gas phase of the protoplanetary disk. The formation process of terrestrial planets in the habitable zone (HZ) and their final water contents are also topics of special interest in this work. Methods. We developed two different sets of N-body simulations starting with the same protoplanetary disk. The first set assumes typical ad hoc initial distributions for embryos and planetesimals, and the second set obtains these initial distributions from the results of a semi-analytical model that simulates the evolution of the protoplanetary disk during the gaseous phase. Results. The two sets of simulations form planets within the HZ. Using ad hoc initial conditions, the masses of the planets that remain in the HZ range from 0.66 M⊕ to 2.27 M⊕. Using more realistic initial conditions obtained from a semi-analytical model, we found that the masses of the planets range from 1.18 M⊕ to 2.21 M⊕. Both sets of simulations form planets in the HZ with water contents ranging between 4.5% and 39.48% by mass. The planets that have the highest water contents with respect to those with the lowest water contents present differences regarding the sources of water supply. Conclusions. From comparing the two sets of simulations, we suggest that the number of planets that remain in the HZ is not sensitive to the particular initial distribution of embryos and planetesimals, and therefore the results are globally similar between them. However, the main differences observed between the two sets are associated with the accretion history of the planets in the HZ. These discrepancies have a direct impact on the accretion of water-rich material and the physical characteristics of the resulting planets.
Fil: Ronco, María Paula. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina
Fil: de Elia, Gonzalo Carlos. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Guilera, Octavio Miguel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina - Materia
-
Astrobiology
NUmerical methods
Protoplanetary disks
Planets formation - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/13780
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Terrestrial-type planet formation. Comparing different types of initial conditionsRonco, María Paulade Elia, Gonzalo CarlosGuilera, Octavio MiguelAstrobiologyNUmerical methodsProtoplanetary disksPlanets formationhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The initial distributions of planetary embryos and planetesimals used in N-body simulations play an important role for studies of the terrestrial-type planet formation during the post oligarchic growth. In general, most of these studies typically use ad hoc initial distributions based primarily on theoretical and numerical studies. Aims. We analyze the formation of planetary systems without gas giants around solar-type stars by focusing on the sensitivity of the results to the particular initial distributions used for planetesimals and planetary embryos at the end of the gas phase of the protoplanetary disk. The formation process of terrestrial planets in the habitable zone (HZ) and their final water contents are also topics of special interest in this work. Methods. We developed two different sets of N-body simulations starting with the same protoplanetary disk. The first set assumes typical ad hoc initial distributions for embryos and planetesimals, and the second set obtains these initial distributions from the results of a semi-analytical model that simulates the evolution of the protoplanetary disk during the gaseous phase. Results. The two sets of simulations form planets within the HZ. Using ad hoc initial conditions, the masses of the planets that remain in the HZ range from 0.66 M⊕ to 2.27 M⊕. Using more realistic initial conditions obtained from a semi-analytical model, we found that the masses of the planets range from 1.18 M⊕ to 2.21 M⊕. Both sets of simulations form planets in the HZ with water contents ranging between 4.5% and 39.48% by mass. The planets that have the highest water contents with respect to those with the lowest water contents present differences regarding the sources of water supply. Conclusions. From comparing the two sets of simulations, we suggest that the number of planets that remain in the HZ is not sensitive to the particular initial distribution of embryos and planetesimals, and therefore the results are globally similar between them. However, the main differences observed between the two sets are associated with the accretion history of the planets in the HZ. These discrepancies have a direct impact on the accretion of water-rich material and the physical characteristics of the resulting planets.Fil: Ronco, María Paula. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; ArgentinaFil: de Elia, Gonzalo Carlos. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Guilera, Octavio Miguel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaEdp Sciences2015-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/13780Ronco, María Paula; de Elia, Gonzalo Carlos; Guilera, Octavio Miguel; Terrestrial-type planet formation. Comparing different types of initial conditions; Edp Sciences; Astronomy And Astrophysics; 584; 47; 12-2015; 1-130004-6361enginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201526367info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/12/aa26367-15/aa26367-15.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:53:04Zoai:ri.conicet.gov.ar:11336/13780instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:53:04.686CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Terrestrial-type planet formation. Comparing different types of initial conditions |
title |
Terrestrial-type planet formation. Comparing different types of initial conditions |
spellingShingle |
Terrestrial-type planet formation. Comparing different types of initial conditions Ronco, María Paula Astrobiology NUmerical methods Protoplanetary disks Planets formation |
title_short |
Terrestrial-type planet formation. Comparing different types of initial conditions |
title_full |
Terrestrial-type planet formation. Comparing different types of initial conditions |
title_fullStr |
Terrestrial-type planet formation. Comparing different types of initial conditions |
title_full_unstemmed |
Terrestrial-type planet formation. Comparing different types of initial conditions |
title_sort |
Terrestrial-type planet formation. Comparing different types of initial conditions |
dc.creator.none.fl_str_mv |
Ronco, María Paula de Elia, Gonzalo Carlos Guilera, Octavio Miguel |
author |
Ronco, María Paula |
author_facet |
Ronco, María Paula de Elia, Gonzalo Carlos Guilera, Octavio Miguel |
author_role |
author |
author2 |
de Elia, Gonzalo Carlos Guilera, Octavio Miguel |
author2_role |
author author |
dc.subject.none.fl_str_mv |
Astrobiology NUmerical methods Protoplanetary disks Planets formation |
topic |
Astrobiology NUmerical methods Protoplanetary disks Planets formation |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Context. The initial distributions of planetary embryos and planetesimals used in N-body simulations play an important role for studies of the terrestrial-type planet formation during the post oligarchic growth. In general, most of these studies typically use ad hoc initial distributions based primarily on theoretical and numerical studies. Aims. We analyze the formation of planetary systems without gas giants around solar-type stars by focusing on the sensitivity of the results to the particular initial distributions used for planetesimals and planetary embryos at the end of the gas phase of the protoplanetary disk. The formation process of terrestrial planets in the habitable zone (HZ) and their final water contents are also topics of special interest in this work. Methods. We developed two different sets of N-body simulations starting with the same protoplanetary disk. The first set assumes typical ad hoc initial distributions for embryos and planetesimals, and the second set obtains these initial distributions from the results of a semi-analytical model that simulates the evolution of the protoplanetary disk during the gaseous phase. Results. The two sets of simulations form planets within the HZ. Using ad hoc initial conditions, the masses of the planets that remain in the HZ range from 0.66 M⊕ to 2.27 M⊕. Using more realistic initial conditions obtained from a semi-analytical model, we found that the masses of the planets range from 1.18 M⊕ to 2.21 M⊕. Both sets of simulations form planets in the HZ with water contents ranging between 4.5% and 39.48% by mass. The planets that have the highest water contents with respect to those with the lowest water contents present differences regarding the sources of water supply. Conclusions. From comparing the two sets of simulations, we suggest that the number of planets that remain in the HZ is not sensitive to the particular initial distribution of embryos and planetesimals, and therefore the results are globally similar between them. However, the main differences observed between the two sets are associated with the accretion history of the planets in the HZ. These discrepancies have a direct impact on the accretion of water-rich material and the physical characteristics of the resulting planets. Fil: Ronco, María Paula. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina Fil: de Elia, Gonzalo Carlos. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Guilera, Octavio Miguel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina |
description |
Context. The initial distributions of planetary embryos and planetesimals used in N-body simulations play an important role for studies of the terrestrial-type planet formation during the post oligarchic growth. In general, most of these studies typically use ad hoc initial distributions based primarily on theoretical and numerical studies. Aims. We analyze the formation of planetary systems without gas giants around solar-type stars by focusing on the sensitivity of the results to the particular initial distributions used for planetesimals and planetary embryos at the end of the gas phase of the protoplanetary disk. The formation process of terrestrial planets in the habitable zone (HZ) and their final water contents are also topics of special interest in this work. Methods. We developed two different sets of N-body simulations starting with the same protoplanetary disk. The first set assumes typical ad hoc initial distributions for embryos and planetesimals, and the second set obtains these initial distributions from the results of a semi-analytical model that simulates the evolution of the protoplanetary disk during the gaseous phase. Results. The two sets of simulations form planets within the HZ. Using ad hoc initial conditions, the masses of the planets that remain in the HZ range from 0.66 M⊕ to 2.27 M⊕. Using more realistic initial conditions obtained from a semi-analytical model, we found that the masses of the planets range from 1.18 M⊕ to 2.21 M⊕. Both sets of simulations form planets in the HZ with water contents ranging between 4.5% and 39.48% by mass. The planets that have the highest water contents with respect to those with the lowest water contents present differences regarding the sources of water supply. Conclusions. From comparing the two sets of simulations, we suggest that the number of planets that remain in the HZ is not sensitive to the particular initial distribution of embryos and planetesimals, and therefore the results are globally similar between them. However, the main differences observed between the two sets are associated with the accretion history of the planets in the HZ. These discrepancies have a direct impact on the accretion of water-rich material and the physical characteristics of the resulting planets. |
publishDate |
2015 |
dc.date.none.fl_str_mv |
2015-12 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/13780 Ronco, María Paula; de Elia, Gonzalo Carlos; Guilera, Octavio Miguel; Terrestrial-type planet formation. Comparing different types of initial conditions; Edp Sciences; Astronomy And Astrophysics; 584; 47; 12-2015; 1-13 0004-6361 |
url |
http://hdl.handle.net/11336/13780 |
identifier_str_mv |
Ronco, María Paula; de Elia, Gonzalo Carlos; Guilera, Octavio Miguel; Terrestrial-type planet formation. Comparing different types of initial conditions; Edp Sciences; Astronomy And Astrophysics; 584; 47; 12-2015; 1-13 0004-6361 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201526367 info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/12/aa26367-15/aa26367-15.html |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
Edp Sciences |
publisher.none.fl_str_mv |
Edp Sciences |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
reponame_str |
CONICET Digital (CONICET) |
collection |
CONICET Digital (CONICET) |
instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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1844613624499273728 |
score |
13.070432 |