Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region

Autores
Parisi, Mirta Gabriela; Valle, Luciano del
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Current models of the formation of ice giants attempt to account for the formation of Uranus and Neptune within the protoplanetary disk lifetime. Many of these models calculate the formation of Uranus and Neptune in a disk that may be several times the minimum mass solar nebula model (MMSN). Modern core accretion theories assume the formation of the ice giants either in situ, or between ~10–20 AU in the framework of the Nice model. However, at present, none of these models account for the spin properties of the ice giants. Aims. Stochastic impacts by large bodies are, at present, the usually accepted mechanisms able to account for the obliquity of the ice giants. We attempt to set constraints on giant impacts as the cause of Neptune’s current obliquity in the framework of modern theories. We also use the present orbital properties of the Neptunian irregular satellites (with the exception of Triton) to set constraints on the scenario of giant impacts at the end of Neptune formation. Methods. Since stochastic collisions among embryos are assumed to occur beyond oligarchy, we model the angular momentum transfer to proto-Neptune and the impulse transfer to its irregular satellites by the last stochastic collision (GC) between the protoplanet and an oligarchic mass at the end of Neptune’s formation. We assume a minimum oligarchic mass mi of 1 m⊕. Results. From angular momentum considerations, we obtain that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 4 m⊕ would be required at the GC to reproduce the present rotational properties of Neptune. An impact with mi > 4 m⊕ is not possible, unless the impact parameter of the collision were very small. This result is invariant either Neptune had formed in situ or between 10–20 AU and does not depend on the occurrence of the GC after or during the possible migration of the planet. From impulse considerations, we find that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 1.4 m⊕ at the GC is required to keep or capture the present population of irregular satellites. If mi had been higher, the present Neptunian irregular satellites had to be formed or captured after the end of stochastic impacts. Conclusions. The upper bounds on the oligarchic masses (4 m⊕ from the obliquity of Neptune and 1.4 m⊕ from the Neptunian irregular satellites) are independent of unknown parameters, such as the mass and distribution of the planetesimals, the location at which Uranus and Neptune were formed, the Solar Nebula initial surface mass density, and the growth regime. If stochastic impacts had occurred, these results should be understood as upper constraints on the oligarchic masses in the trans-Saturnian region at the end of ice planet formation and may be used to set constraints on planetary formation scenarios.
Fil: Parisi, Mirta Gabriela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Valle, Luciano del. Universidad Austral de Chile; Chile
Materia
Planets
Satellites
Satellite formation
Planets formation
Nivel de accesibilidad
acceso abierto
Condiciones de uso
Atribución-NoComercial-CompartirIgual 2.5 Argentina (CC 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:11336/4635

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oai_identifier_str oai:ri.conicet.gov.ar:11336/4635
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network_name_str CONICET Digital (CONICET)
spelling Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian regionParisi, Mirta GabrielaValle, Luciano delPlanetsSatellitesSatellite formationPlanets formationhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Current models of the formation of ice giants attempt to account for the formation of Uranus and Neptune within the protoplanetary disk lifetime. Many of these models calculate the formation of Uranus and Neptune in a disk that may be several times the minimum mass solar nebula model (MMSN). Modern core accretion theories assume the formation of the ice giants either in situ, or between ~10–20 AU in the framework of the Nice model. However, at present, none of these models account for the spin properties of the ice giants. Aims. Stochastic impacts by large bodies are, at present, the usually accepted mechanisms able to account for the obliquity of the ice giants. We attempt to set constraints on giant impacts as the cause of Neptune’s current obliquity in the framework of modern theories. We also use the present orbital properties of the Neptunian irregular satellites (with the exception of Triton) to set constraints on the scenario of giant impacts at the end of Neptune formation. Methods. Since stochastic collisions among embryos are assumed to occur beyond oligarchy, we model the angular momentum transfer to proto-Neptune and the impulse transfer to its irregular satellites by the last stochastic collision (GC) between the protoplanet and an oligarchic mass at the end of Neptune’s formation. We assume a minimum oligarchic mass mi of 1 m⊕. Results. From angular momentum considerations, we obtain that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 4 m⊕ would be required at the GC to reproduce the present rotational properties of Neptune. An impact with mi > 4 m⊕ is not possible, unless the impact parameter of the collision were very small. This result is invariant either Neptune had formed in situ or between 10–20 AU and does not depend on the occurrence of the GC after or during the possible migration of the planet. From impulse considerations, we find that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 1.4 m⊕ at the GC is required to keep or capture the present population of irregular satellites. If mi had been higher, the present Neptunian irregular satellites had to be formed or captured after the end of stochastic impacts. Conclusions. The upper bounds on the oligarchic masses (4 m⊕ from the obliquity of Neptune and 1.4 m⊕ from the Neptunian irregular satellites) are independent of unknown parameters, such as the mass and distribution of the planetesimals, the location at which Uranus and Neptune were formed, the Solar Nebula initial surface mass density, and the growth regime. If stochastic impacts had occurred, these results should be understood as upper constraints on the oligarchic masses in the trans-Saturnian region at the end of ice planet formation and may be used to set constraints on planetary formation scenarios.Fil: Parisi, Mirta Gabriela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Valle, Luciano del. Universidad Austral de Chile; ChileEDP Sciences2011-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/4635Parisi, Mirta Gabriela; Valle, Luciano del; Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region; EDP Sciences; Astronomy and Astrophysics; 530; A46; 2-2011; 1-110004-6361enginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201016282info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2011/06/aa16282-10/aa16282-10.htmlinfo:eu-repo/semantics/openAccessAtribución-NoComercial-CompartirIgual 2.5 Argentina (CC BY-NC-SA 2.5 AR)https://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:45:50Zoai:ri.conicet.gov.ar:11336/4635instacron: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 09:45:50.399CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region
title Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region
spellingShingle Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region
Parisi, Mirta Gabriela
Planets
Satellites
Satellite formation
Planets formation
title_short Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region
title_full Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region
title_fullStr Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region
title_full_unstemmed Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region
title_sort Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region
dc.creator.none.fl_str_mv Parisi, Mirta Gabriela
Valle, Luciano del
author Parisi, Mirta Gabriela
author_facet Parisi, Mirta Gabriela
Valle, Luciano del
author_role author
author2 Valle, Luciano del
author2_role author
dc.subject.none.fl_str_mv Planets
Satellites
Satellite formation
Planets formation
topic Planets
Satellites
Satellite formation
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. Current models of the formation of ice giants attempt to account for the formation of Uranus and Neptune within the protoplanetary disk lifetime. Many of these models calculate the formation of Uranus and Neptune in a disk that may be several times the minimum mass solar nebula model (MMSN). Modern core accretion theories assume the formation of the ice giants either in situ, or between ~10–20 AU in the framework of the Nice model. However, at present, none of these models account for the spin properties of the ice giants. Aims. Stochastic impacts by large bodies are, at present, the usually accepted mechanisms able to account for the obliquity of the ice giants. We attempt to set constraints on giant impacts as the cause of Neptune’s current obliquity in the framework of modern theories. We also use the present orbital properties of the Neptunian irregular satellites (with the exception of Triton) to set constraints on the scenario of giant impacts at the end of Neptune formation. Methods. Since stochastic collisions among embryos are assumed to occur beyond oligarchy, we model the angular momentum transfer to proto-Neptune and the impulse transfer to its irregular satellites by the last stochastic collision (GC) between the protoplanet and an oligarchic mass at the end of Neptune’s formation. We assume a minimum oligarchic mass mi of 1 m⊕. Results. From angular momentum considerations, we obtain that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 4 m⊕ would be required at the GC to reproduce the present rotational properties of Neptune. An impact with mi > 4 m⊕ is not possible, unless the impact parameter of the collision were very small. This result is invariant either Neptune had formed in situ or between 10–20 AU and does not depend on the occurrence of the GC after or during the possible migration of the planet. From impulse considerations, we find that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 1.4 m⊕ at the GC is required to keep or capture the present population of irregular satellites. If mi had been higher, the present Neptunian irregular satellites had to be formed or captured after the end of stochastic impacts. Conclusions. The upper bounds on the oligarchic masses (4 m⊕ from the obliquity of Neptune and 1.4 m⊕ from the Neptunian irregular satellites) are independent of unknown parameters, such as the mass and distribution of the planetesimals, the location at which Uranus and Neptune were formed, the Solar Nebula initial surface mass density, and the growth regime. If stochastic impacts had occurred, these results should be understood as upper constraints on the oligarchic masses in the trans-Saturnian region at the end of ice planet formation and may be used to set constraints on planetary formation scenarios.
Fil: Parisi, Mirta Gabriela. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Valle, Luciano del. Universidad Austral de Chile; Chile
description Context. Current models of the formation of ice giants attempt to account for the formation of Uranus and Neptune within the protoplanetary disk lifetime. Many of these models calculate the formation of Uranus and Neptune in a disk that may be several times the minimum mass solar nebula model (MMSN). Modern core accretion theories assume the formation of the ice giants either in situ, or between ~10–20 AU in the framework of the Nice model. However, at present, none of these models account for the spin properties of the ice giants. Aims. Stochastic impacts by large bodies are, at present, the usually accepted mechanisms able to account for the obliquity of the ice giants. We attempt to set constraints on giant impacts as the cause of Neptune’s current obliquity in the framework of modern theories. We also use the present orbital properties of the Neptunian irregular satellites (with the exception of Triton) to set constraints on the scenario of giant impacts at the end of Neptune formation. Methods. Since stochastic collisions among embryos are assumed to occur beyond oligarchy, we model the angular momentum transfer to proto-Neptune and the impulse transfer to its irregular satellites by the last stochastic collision (GC) between the protoplanet and an oligarchic mass at the end of Neptune’s formation. We assume a minimum oligarchic mass mi of 1 m⊕. Results. From angular momentum considerations, we obtain that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 4 m⊕ would be required at the GC to reproduce the present rotational properties of Neptune. An impact with mi > 4 m⊕ is not possible, unless the impact parameter of the collision were very small. This result is invariant either Neptune had formed in situ or between 10–20 AU and does not depend on the occurrence of the GC after or during the possible migration of the planet. From impulse considerations, we find that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 1.4 m⊕ at the GC is required to keep or capture the present population of irregular satellites. If mi had been higher, the present Neptunian irregular satellites had to be formed or captured after the end of stochastic impacts. Conclusions. The upper bounds on the oligarchic masses (4 m⊕ from the obliquity of Neptune and 1.4 m⊕ from the Neptunian irregular satellites) are independent of unknown parameters, such as the mass and distribution of the planetesimals, the location at which Uranus and Neptune were formed, the Solar Nebula initial surface mass density, and the growth regime. If stochastic impacts had occurred, these results should be understood as upper constraints on the oligarchic masses in the trans-Saturnian region at the end of ice planet formation and may be used to set constraints on planetary formation scenarios.
publishDate 2011
dc.date.none.fl_str_mv 2011-02
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/11336/4635
Parisi, Mirta Gabriela; Valle, Luciano del; Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region; EDP Sciences; Astronomy and Astrophysics; 530; A46; 2-2011; 1-11
0004-6361
url http://hdl.handle.net/11336/4635
identifier_str_mv Parisi, Mirta Gabriela; Valle, Luciano del; Last giant impact on the Neptunian System : constraints on oligarchic masses in the trans-Saturnian region; EDP Sciences; Astronomy and Astrophysics; 530; A46; 2-2011; 1-11
0004-6361
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201016282
info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2011/06/aa16282-10/aa16282-10.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
Atribución-NoComercial-CompartirIgual 2.5 Argentina (CC BY-NC-SA 2.5 AR)
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv Atribución-NoComercial-CompartirIgual 2.5 Argentina (CC BY-NC-SA 2.5 AR)
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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