The Irregular Satellites of Neptune: a window to the Young Solar System

Autores
Parisi, Mirta Gabriela; del Valle, Luciano Noe
Año de publicación
2009
Idioma
inglés
Tipo de recurso
documento de conferencia
Estado
versión publicada
Descripción
The origin of planetary rotation and obliquity is one of the fundamental questions of Cosmogony, and also has proven to be one of the most difficult to answer. Although the obliquity of the giant planets remains an openned question, it is believed that it might be due to stochastic processes at the end of the accretionary epoch (e. g., Safronov 1969). If satellites had been orbiting around giant planets before large impacts had taken place, the impulse imparted at collision would have produced a shift in the orbital velocity of the satellites. Then, the present physical and dynamical properties of the irregular satellites of giant planets are used to set constraints on the scenario of giant impacts at the end of the formation of the Solar System, which implies contraints on models of planetary formation.     For the case of Uranus, constraints on the stochastic processes as the cause of the large obliquity of Uranus, physical conditions for this planet, dynamical constraints and restrictions on the possible mechanisms for the origin of the irregular Uranian satellites were obtained from the knowledge of the actual physical and orbital properties of these satellites (Parisi and Brunini 1997, Brunini et al. 2002, Maris et al. 2007, Parisi et al. 2008).     Motivated by our results for the Uranian system, we carried out the firstmodel of a giant impact on Neptune as the cause of this planet obliquity and set constraints on this scenario from the orbital properties of the Neptunian irregular satellites. In order to get the physical properties of these satellites, we start an observing program using FORS2 at ESO-VLT (ESO program 083.C-0526, PI: Maris). These observations will allow us to derive by first time their colors, which are the best source of information to know their relation to the precursor Kuiper Belt population, posing contraints on their origin, formation mechanism and models of planetary formation.
Fil: Parisi, Mirta Gabriela. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: del Valle, Luciano Noe. Universidad de Chile; Chile
IAU Symposium 263: Icy Bodies of the Solar System
Río de Janeiro
Brasil
International Astronomical Union
Materia
Planets and Satellites: general
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:11336/232207

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spelling The Irregular Satellites of Neptune: a window to the Young Solar SystemParisi, Mirta Gabrieladel Valle, Luciano NoePlanets and Satellites: generalhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The origin of planetary rotation and obliquity is one of the fundamental questions of Cosmogony, and also has proven to be one of the most difficult to answer. Although the obliquity of the giant planets remains an openned question, it is believed that it might be due to stochastic processes at the end of the accretionary epoch (e. g., Safronov 1969). If satellites had been orbiting around giant planets before large impacts had taken place, the impulse imparted at collision would have produced a shift in the orbital velocity of the satellites. Then, the present physical and dynamical properties of the irregular satellites of giant planets are used to set constraints on the scenario of giant impacts at the end of the formation of the Solar System, which implies contraints on models of planetary formation.     For the case of Uranus, constraints on the stochastic processes as the cause of the large obliquity of Uranus, physical conditions for this planet, dynamical constraints and restrictions on the possible mechanisms for the origin of the irregular Uranian satellites were obtained from the knowledge of the actual physical and orbital properties of these satellites (Parisi and Brunini 1997, Brunini et al. 2002, Maris et al. 2007, Parisi et al. 2008).     Motivated by our results for the Uranian system, we carried out the firstmodel of a giant impact on Neptune as the cause of this planet obliquity and set constraints on this scenario from the orbital properties of the Neptunian irregular satellites. In order to get the physical properties of these satellites, we start an observing program using FORS2 at ESO-VLT (ESO program 083.C-0526, PI: Maris). These observations will allow us to derive by first time their colors, which are the best source of information to know their relation to the precursor Kuiper Belt population, posing contraints on their origin, formation mechanism and models of planetary formation.Fil: Parisi, Mirta Gabriela. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: del Valle, Luciano Noe. Universidad de Chile; ChileIAU Symposium 263: Icy Bodies of the Solar SystemRío de JaneiroBrasilInternational Astronomical UnionCambridge University PressFernandez, Julio A.Lazzaro, DanielaPrialnik, DinaSchulz, Rita2009info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectSimposioJournalhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/232207The Irregular Satellites of Neptune: a window to the Young Solar System; IAU Symposium 263: Icy Bodies of the Solar System; Río de Janeiro; Brasil; 2009; 54-549780521764889CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://www.astronomia.edu.uy/congresos/symp263/symp263_program.htminfo:eu-repo/semantics/altIdentifier/url/http://www.astronomia.edu.uy/congresos/symp263/info:eu-repo/semantics/altIdentifier/url/https://inspirehep.net/conferences/1406610Internacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:44:20Zoai:ri.conicet.gov.ar:11336/232207instacron: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 09:44:20.622CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The Irregular Satellites of Neptune: a window to the Young Solar System
title The Irregular Satellites of Neptune: a window to the Young Solar System
spellingShingle The Irregular Satellites of Neptune: a window to the Young Solar System
Parisi, Mirta Gabriela
Planets and Satellites: general
title_short The Irregular Satellites of Neptune: a window to the Young Solar System
title_full The Irregular Satellites of Neptune: a window to the Young Solar System
title_fullStr The Irregular Satellites of Neptune: a window to the Young Solar System
title_full_unstemmed The Irregular Satellites of Neptune: a window to the Young Solar System
title_sort The Irregular Satellites of Neptune: a window to the Young Solar System
dc.creator.none.fl_str_mv Parisi, Mirta Gabriela
del Valle, Luciano Noe
author Parisi, Mirta Gabriela
author_facet Parisi, Mirta Gabriela
del Valle, Luciano Noe
author_role author
author2 del Valle, Luciano Noe
author2_role author
dc.contributor.none.fl_str_mv Fernandez, Julio A.
Lazzaro, Daniela
Prialnik, Dina
Schulz, Rita
dc.subject.none.fl_str_mv Planets and Satellites: general
topic Planets and Satellites: general
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The origin of planetary rotation and obliquity is one of the fundamental questions of Cosmogony, and also has proven to be one of the most difficult to answer. Although the obliquity of the giant planets remains an openned question, it is believed that it might be due to stochastic processes at the end of the accretionary epoch (e. g., Safronov 1969). If satellites had been orbiting around giant planets before large impacts had taken place, the impulse imparted at collision would have produced a shift in the orbital velocity of the satellites. Then, the present physical and dynamical properties of the irregular satellites of giant planets are used to set constraints on the scenario of giant impacts at the end of the formation of the Solar System, which implies contraints on models of planetary formation.     For the case of Uranus, constraints on the stochastic processes as the cause of the large obliquity of Uranus, physical conditions for this planet, dynamical constraints and restrictions on the possible mechanisms for the origin of the irregular Uranian satellites were obtained from the knowledge of the actual physical and orbital properties of these satellites (Parisi and Brunini 1997, Brunini et al. 2002, Maris et al. 2007, Parisi et al. 2008).     Motivated by our results for the Uranian system, we carried out the firstmodel of a giant impact on Neptune as the cause of this planet obliquity and set constraints on this scenario from the orbital properties of the Neptunian irregular satellites. In order to get the physical properties of these satellites, we start an observing program using FORS2 at ESO-VLT (ESO program 083.C-0526, PI: Maris). These observations will allow us to derive by first time their colors, which are the best source of information to know their relation to the precursor Kuiper Belt population, posing contraints on their origin, formation mechanism and models of planetary formation.
Fil: Parisi, Mirta Gabriela. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: del Valle, Luciano Noe. Universidad de Chile; Chile
IAU Symposium 263: Icy Bodies of the Solar System
Río de Janeiro
Brasil
International Astronomical Union
description The origin of planetary rotation and obliquity is one of the fundamental questions of Cosmogony, and also has proven to be one of the most difficult to answer. Although the obliquity of the giant planets remains an openned question, it is believed that it might be due to stochastic processes at the end of the accretionary epoch (e. g., Safronov 1969). If satellites had been orbiting around giant planets before large impacts had taken place, the impulse imparted at collision would have produced a shift in the orbital velocity of the satellites. Then, the present physical and dynamical properties of the irregular satellites of giant planets are used to set constraints on the scenario of giant impacts at the end of the formation of the Solar System, which implies contraints on models of planetary formation.     For the case of Uranus, constraints on the stochastic processes as the cause of the large obliquity of Uranus, physical conditions for this planet, dynamical constraints and restrictions on the possible mechanisms for the origin of the irregular Uranian satellites were obtained from the knowledge of the actual physical and orbital properties of these satellites (Parisi and Brunini 1997, Brunini et al. 2002, Maris et al. 2007, Parisi et al. 2008).     Motivated by our results for the Uranian system, we carried out the firstmodel of a giant impact on Neptune as the cause of this planet obliquity and set constraints on this scenario from the orbital properties of the Neptunian irregular satellites. In order to get the physical properties of these satellites, we start an observing program using FORS2 at ESO-VLT (ESO program 083.C-0526, PI: Maris). These observations will allow us to derive by first time their colors, which are the best source of information to know their relation to the precursor Kuiper Belt population, posing contraints on their origin, formation mechanism and models of planetary formation.
publishDate 2009
dc.date.none.fl_str_mv 2009
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The Irregular Satellites of Neptune: a window to the Young Solar System; IAU Symposium 263: Icy Bodies of the Solar System; Río de Janeiro; Brasil; 2009; 54-54
9780521764889
CONICET Digital
CONICET
url http://hdl.handle.net/11336/232207
identifier_str_mv The Irregular Satellites of Neptune: a window to the Young Solar System; IAU Symposium 263: Icy Bodies of the Solar System; Río de Janeiro; Brasil; 2009; 54-54
9780521764889
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
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info:eu-repo/semantics/altIdentifier/url/https://inspirehep.net/conferences/1406610
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dc.coverage.none.fl_str_mv Internacional
dc.publisher.none.fl_str_mv Cambridge University Press
publisher.none.fl_str_mv Cambridge University Press
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