Last giant impact on the Neptunian system: Constraints on oligarchic masses in the trans-Saturnian region

Autores
Parisi, Mirta Gabriela; Valle, L. 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 mSUB>i > 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.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
Materia
Ciencias Astronómicas
Planets and satellites: formation
Planets and satellites: general
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:10915/83996

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/83996
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Last giant impact on the Neptunian system: Constraints on oligarchic masses in the trans-Saturnian regionParisi, Mirta GabrielaValle, L. delCiencias AstronómicasPlanets and satellites: formationPlanets and satellites: generalContext. 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 m<SUB>i</SUB> of 1 m<SUB>⊕</SUB>. Results. From angular momentum considerations, we obtain that an oligarchic mass m<SUB>i</SUB> ∼ 1 m<SUB>⊕</SUB> = m<SUB>i</SUB> = 4 m<SUB>⊕</SUB> would be required at the GC to reproduce the present rotational properties of Neptune. An impact with mSUB>i</SUB> > 4 m<SUB>⊕</SUB> 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 m<SUB>i</SUB> ∼ 1 m<SUB>⊕</SUB> = m<SUB>i</SUB> = 1.4 m<SUB>⊕</SUB> at the GC is required to keep or capture the present population of irregular satellites. If m<SUB>i</SUB> 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<SUB>⊕</SUB> from the obliquity of Neptune and 1.4 m<SUB>⊕</SUB> 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.Facultad de Ciencias Astronómicas y GeofísicasInstituto Argentino de Radioastronomía2011info: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/10915/83996enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201016282info: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:UNLP2025-09-29T11:16:10Zoai:sedici.unlp.edu.ar:10915/83996Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:10.277SEDICI (UNLP) - Universidad Nacional de La Platafalse
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
Ciencias Astronómicas
Planets and satellites: formation
Planets and satellites: general
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, L. del
author Parisi, Mirta Gabriela
author_facet Parisi, Mirta Gabriela
Valle, L. del
author_role author
author2 Valle, L. del
author2_role author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Planets and satellites: formation
Planets and satellites: general
topic Ciencias Astronómicas
Planets and satellites: formation
Planets and satellites: general
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 m<SUB>i</SUB> of 1 m<SUB>⊕</SUB>. Results. From angular momentum considerations, we obtain that an oligarchic mass m<SUB>i</SUB> ∼ 1 m<SUB>⊕</SUB> = m<SUB>i</SUB> = 4 m<SUB>⊕</SUB> would be required at the GC to reproduce the present rotational properties of Neptune. An impact with mSUB>i</SUB> > 4 m<SUB>⊕</SUB> 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 m<SUB>i</SUB> ∼ 1 m<SUB>⊕</SUB> = m<SUB>i</SUB> = 1.4 m<SUB>⊕</SUB> at the GC is required to keep or capture the present population of irregular satellites. If m<SUB>i</SUB> 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<SUB>⊕</SUB> from the obliquity of Neptune and 1.4 m<SUB>⊕</SUB> 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.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
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 m<SUB>i</SUB> of 1 m<SUB>⊕</SUB>. Results. From angular momentum considerations, we obtain that an oligarchic mass m<SUB>i</SUB> ∼ 1 m<SUB>⊕</SUB> = m<SUB>i</SUB> = 4 m<SUB>⊕</SUB> would be required at the GC to reproduce the present rotational properties of Neptune. An impact with mSUB>i</SUB> > 4 m<SUB>⊕</SUB> 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 m<SUB>i</SUB> ∼ 1 m<SUB>⊕</SUB> = m<SUB>i</SUB> = 1.4 m<SUB>⊕</SUB> at the GC is required to keep or capture the present population of irregular satellites. If m<SUB>i</SUB> 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<SUB>⊕</SUB> from the obliquity of Neptune and 1.4 m<SUB>⊕</SUB> 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
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info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201016282
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Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
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rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
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