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

Autores
Ronco, María Paula; Elía, Gonzalo Carlos de
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 (HZ) and analyze their water contents with the goal to determine systems of astrobiological interest. In addition, 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-γ, with an exponential decay to the outside. We performed simulations adopting a disk of 0.03 M ⊙ and values of γ = 0.5, 1 and 1.5. Results. All our simulations form planets in the HZ with different masses and final water contents depending on the three different profiles. For γ = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 MŠ to 0.1 M⊕ and water contents between 0.2 and 16 Earth oceans (1 Earth ocean =2.8 × 10-4⊕). For γ = 1, three planets form in the HZ with masses between 0.18 M⊕ and 0.52 M⊕ and water contents from 34 to 167 Earth oceans. Finally, for γ = 1.5, we find four planets in the HZ with masses ranging from 0.66 M⊕ to 2.21 M⊕ 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 γ = 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 3 M⊕ around the snow line, which can be discovered by the microlensing technique.
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
Astrobiology
Methods: numerical
Protoplanetary disks
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/85235

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/85235
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Diversity of planetary systems in low-mass disks: terrestrial-type planet formation and water deliveryRonco, María PaulaElía, Gonzalo Carlos deCiencias AstronómicasAstrobiologyMethods: numericalProtoplanetary disks<b>Context.</b> Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe. <b>Aims.</b> 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 (HZ) and analyze their water contents with the goal to determine systems of astrobiological interest. In addition, we study the formation of planets on wide orbits because they can be detected with the microlensing technique. <b>Methods.</b> 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-γ, with an exponential decay to the outside. We performed simulations adopting a disk of 0.03 M ⊙ and values of γ = 0.5, 1 and 1.5. <b>Results.</b> All our simulations form planets in the HZ with different masses and final water contents depending on the three different profiles. For γ = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 MŠ to 0.1 M⊕ and water contents between 0.2 and 16 Earth oceans (1 Earth ocean =2.8 × 10-4⊕). For γ = 1, three planets form in the HZ with masses between 0.18 M⊕ and 0.52 M⊕ and water contents from 34 to 167 Earth oceans. Finally, for γ = 1.5, we find four planets in the HZ with masses ranging from 0.66 M⊕ to 2.21 M⊕ 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. <b>Conclusions.</b> Since planetary systems with γ = 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 3 M⊕ around the snow line, which can be discovered by the microlensing technique.Instituto de Astrofísica de La Plata2014-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/85235enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201323313info: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:UNLP2025-09-29T11:16:24Zoai:sedici.unlp.edu.ar:10915/85235Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:25.147SEDICI (UNLP) - Universidad Nacional de La Platafalse
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
Ciencias Astronómicas
Astrobiology
Methods: numerical
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
Elía, Gonzalo Carlos de
author Ronco, María Paula
author_facet Ronco, María Paula
Elía, Gonzalo Carlos de
author_role author
author2 Elía, Gonzalo Carlos de
author2_role author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Astrobiology
Methods: numerical
Protoplanetary disks
topic Ciencias Astronómicas
Astrobiology
Methods: numerical
Protoplanetary disks
dc.description.none.fl_txt_mv <b>Context.</b> Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe. <b>Aims.</b> 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 (HZ) and analyze their water contents with the goal to determine systems of astrobiological interest. In addition, we study the formation of planets on wide orbits because they can be detected with the microlensing technique. <b>Methods.</b> 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-γ, with an exponential decay to the outside. We performed simulations adopting a disk of 0.03 M ⊙ and values of γ = 0.5, 1 and 1.5. <b>Results.</b> All our simulations form planets in the HZ with different masses and final water contents depending on the three different profiles. For γ = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 MŠ to 0.1 M⊕ and water contents between 0.2 and 16 Earth oceans (1 Earth ocean =2.8 × 10-4⊕). For γ = 1, three planets form in the HZ with masses between 0.18 M⊕ and 0.52 M⊕ and water contents from 34 to 167 Earth oceans. Finally, for γ = 1.5, we find four planets in the HZ with masses ranging from 0.66 M⊕ to 2.21 M⊕ 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. <b>Conclusions.</b> Since planetary systems with γ = 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 3 M⊕ around the snow line, which can be discovered by the microlensing technique.
Instituto de Astrofísica de La Plata
description <b>Context.</b> Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe. <b>Aims.</b> 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 (HZ) and analyze their water contents with the goal to determine systems of astrobiological interest. In addition, we study the formation of planets on wide orbits because they can be detected with the microlensing technique. <b>Methods.</b> 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-γ, with an exponential decay to the outside. We performed simulations adopting a disk of 0.03 M ⊙ and values of γ = 0.5, 1 and 1.5. <b>Results.</b> All our simulations form planets in the HZ with different masses and final water contents depending on the three different profiles. For γ = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 MŠ to 0.1 M⊕ and water contents between 0.2 and 16 Earth oceans (1 Earth ocean =2.8 × 10-4⊕). For γ = 1, three planets form in the HZ with masses between 0.18 M⊕ and 0.52 M⊕ and water contents from 34 to 167 Earth oceans. Finally, for γ = 1.5, we find four planets in the HZ with masses ranging from 0.66 M⊕ to 2.21 M⊕ 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. <b>Conclusions.</b> Since planetary systems with γ = 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 3 M⊕ around the snow line, which can be discovered by the microlensing technique.
publishDate 2014
dc.date.none.fl_str_mv 2014-07
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info:eu-repo/semantics/publishedVersion
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dc.language.none.fl_str_mv eng
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dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6361
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201323313
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
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