Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery

Autores
Ronco, María Paula; de Elia, Gonzalo Carlos
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe.
Aims. We study the diversity of planetary systems that might form around Sun-like stars in low-mass disks without gas-giant planets. We focus especially on the formation process of terrestrial planets in the habitable zone and analyze their water contents with the goal to determine systems of astrobiological interest. In adittion, we study the formation of planets on wide orbits because they can be detected with the microlensing technique.
Methods. N-body simulations of high resolution were developed for a wide range of surface density profiles. A bimodal distribution of planetesimals and planetary embryos with different physical and orbital configurations was used to simulate the planetary accretion process. The surface density profile combines a power law for the inside of the disk of the form r−gamma , with an exponential decay to the outside. We performed simulations adopting a disk of 0.03Msun and values of   gamma = 0.5, 1 and 1.5.
Results. All our simulations form planets in the habitable zone (HZ) with different masses and final water contents depending on the three different profiles. For gamma  = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 Mearth to 0.1 Mearth and water contents between 0.2 and 16 Earth oceans (1 Earth ocean = 2.8× 10−4 Mearth). For gamma  = 1, three planets form in the HZ with masses between 0.18 Mearth and 0.52 Mearth and water contents from 34 to 167 Earth oceans. Finally, for gamma  = 1.5, we find four planets in the HZ with masses ranging from 0.66 Mearth to 2.21 Mearth and water contents between 192 and 2326 Earth oceans. This profile shows distinctive results because it is the only one of those studied here that leads to the formation of water worlds.
Conclusions. Since planetary systems with  gamma = 1 and 1.5 present planets in the HZ with suitable masses to retain a long-lived atmosphere and to maintain plate tectonics, they seem to be the most promising candidates to be potentially habitable. Particularly, these systems form Earths and Super-Earths of at least 3Mearth around the snow line, which can be discovered by the microlensing technique.
Fil: Ronco, María Paula. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Fil: de Elia, Gonzalo Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Materia
Astrobiology
Numerical Methosd
Protoplanetary Disks
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/35454

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network_name_str CONICET Digital (CONICET)
spelling Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water deliveryRonco, María Paulade Elia, Gonzalo CarlosAstrobiologyNumerical MethosdProtoplanetary Diskshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe.<br />Aims. We study the diversity of planetary systems that might form around Sun-like stars in low-mass disks without gas-giant planets. We focus especially on the formation process of terrestrial planets in the habitable zone and analyze their water contents with the goal to determine systems of astrobiological interest. In adittion, we study the formation of planets on wide orbits because they can be detected with the microlensing technique.<br />Methods. N-body simulations of high resolution were developed for a wide range of surface density profiles. A bimodal distribution of planetesimals and planetary embryos with different physical and orbital configurations was used to simulate the planetary accretion process. The surface density profile combines a power law for the inside of the disk of the form r−gamma , with an exponential decay to the outside. We performed simulations adopting a disk of 0.03Msun and values of   gamma = 0.5, 1 and 1.5.<br />Results. All our simulations form planets in the habitable zone (HZ) with different masses and final water contents depending on the three different profiles. For gamma  = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 Mearth to 0.1 Mearth and water contents between 0.2 and 16 Earth oceans (1 Earth ocean = 2.8× 10−4 Mearth). For gamma  = 1, three planets form in the HZ with masses between 0.18 Mearth and 0.52 Mearth and water contents from 34 to 167 Earth oceans. Finally, for gamma  = 1.5, we find four planets in the HZ with masses ranging from 0.66 Mearth to 2.21 Mearth and water contents between 192 and 2326 Earth oceans. This profile shows distinctive results because it is the only one of those studied here that leads to the formation of water worlds.<br />Conclusions. Since planetary systems with  gamma = 1 and 1.5 present planets in the HZ with suitable masses to retain a long-lived atmosphere and to maintain plate tectonics, they seem to be the most promising candidates to be potentially habitable. Particularly, these systems form Earths and Super-Earths of at least 3Mearth around the snow line, which can be discovered by the microlensing technique.Fil: Ronco, María Paula. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; ArgentinaFil: de Elia, Gonzalo Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; ArgentinaEDP Sciences2014-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/35454Ronco, María Paula; de Elia, Gonzalo Carlos; Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery; EDP Sciences; Astronomy and Astrophysics; 567; A54; 7-2014; 1-130004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201323313info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2014/07/aa23313-13/aa23313-13.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 Técnicas2025-09-29T10:45:48Zoai:ri.conicet.gov.ar:11336/35454instacron: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 10:45:48.722CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
title Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
spellingShingle Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
Ronco, María Paula
Astrobiology
Numerical Methosd
Protoplanetary Disks
title_short Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
title_full Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
title_fullStr Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
title_full_unstemmed Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
title_sort Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
dc.creator.none.fl_str_mv Ronco, María Paula
de Elia, Gonzalo Carlos
author Ronco, María Paula
author_facet Ronco, María Paula
de Elia, Gonzalo Carlos
author_role author
author2 de Elia, Gonzalo Carlos
author2_role author
dc.subject.none.fl_str_mv Astrobiology
Numerical Methosd
Protoplanetary Disks
topic Astrobiology
Numerical Methosd
Protoplanetary Disks
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. Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe.<br />Aims. We study the diversity of planetary systems that might form around Sun-like stars in low-mass disks without gas-giant planets. We focus especially on the formation process of terrestrial planets in the habitable zone and analyze their water contents with the goal to determine systems of astrobiological interest. In adittion, we study the formation of planets on wide orbits because they can be detected with the microlensing technique.<br />Methods. N-body simulations of high resolution were developed for a wide range of surface density profiles. A bimodal distribution of planetesimals and planetary embryos with different physical and orbital configurations was used to simulate the planetary accretion process. The surface density profile combines a power law for the inside of the disk of the form r−gamma , with an exponential decay to the outside. We performed simulations adopting a disk of 0.03Msun and values of   gamma = 0.5, 1 and 1.5.<br />Results. All our simulations form planets in the habitable zone (HZ) with different masses and final water contents depending on the three different profiles. For gamma  = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 Mearth to 0.1 Mearth and water contents between 0.2 and 16 Earth oceans (1 Earth ocean = 2.8× 10−4 Mearth). For gamma  = 1, three planets form in the HZ with masses between 0.18 Mearth and 0.52 Mearth and water contents from 34 to 167 Earth oceans. Finally, for gamma  = 1.5, we find four planets in the HZ with masses ranging from 0.66 Mearth to 2.21 Mearth and water contents between 192 and 2326 Earth oceans. This profile shows distinctive results because it is the only one of those studied here that leads to the formation of water worlds.<br />Conclusions. Since planetary systems with  gamma = 1 and 1.5 present planets in the HZ with suitable masses to retain a long-lived atmosphere and to maintain plate tectonics, they seem to be the most promising candidates to be potentially habitable. Particularly, these systems form Earths and Super-Earths of at least 3Mearth around the snow line, which can be discovered by the microlensing technique.
Fil: Ronco, María Paula. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Fil: de Elia, Gonzalo Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
description Context. Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe.<br />Aims. We study the diversity of planetary systems that might form around Sun-like stars in low-mass disks without gas-giant planets. We focus especially on the formation process of terrestrial planets in the habitable zone and analyze their water contents with the goal to determine systems of astrobiological interest. In adittion, we study the formation of planets on wide orbits because they can be detected with the microlensing technique.<br />Methods. N-body simulations of high resolution were developed for a wide range of surface density profiles. A bimodal distribution of planetesimals and planetary embryos with different physical and orbital configurations was used to simulate the planetary accretion process. The surface density profile combines a power law for the inside of the disk of the form r−gamma , with an exponential decay to the outside. We performed simulations adopting a disk of 0.03Msun and values of   gamma = 0.5, 1 and 1.5.<br />Results. All our simulations form planets in the habitable zone (HZ) with different masses and final water contents depending on the three different profiles. For gamma  = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 Mearth to 0.1 Mearth and water contents between 0.2 and 16 Earth oceans (1 Earth ocean = 2.8× 10−4 Mearth). For gamma  = 1, three planets form in the HZ with masses between 0.18 Mearth and 0.52 Mearth and water contents from 34 to 167 Earth oceans. Finally, for gamma  = 1.5, we find four planets in the HZ with masses ranging from 0.66 Mearth to 2.21 Mearth and water contents between 192 and 2326 Earth oceans. This profile shows distinctive results because it is the only one of those studied here that leads to the formation of water worlds.<br />Conclusions. Since planetary systems with  gamma = 1 and 1.5 present planets in the HZ with suitable masses to retain a long-lived atmosphere and to maintain plate tectonics, they seem to be the most promising candidates to be potentially habitable. Particularly, these systems form Earths and Super-Earths of at least 3Mearth around the snow line, which can be discovered by the microlensing technique.
publishDate 2014
dc.date.none.fl_str_mv 2014-07
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/11336/35454
Ronco, María Paula; de Elia, Gonzalo Carlos; Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery; EDP Sciences; Astronomy and Astrophysics; 567; A54; 7-2014; 1-13
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/35454
identifier_str_mv Ronco, María Paula; de Elia, Gonzalo Carlos; Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery; EDP Sciences; Astronomy and Astrophysics; 567; A54; 7-2014; 1-13
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201323313
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2014/07/aa23313-13/aa23313-13.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
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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
application/pdf
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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)
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repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
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