On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations

Autores
Di Sisto, Romina Paula; Fernández, Julio A.; Brunini, Adrian
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We study the Jupiter family comet (JFC) population assumed to come from the Scattered Disk and transferred to the Jupiter’s zone through gravitational interactions with the Jovian planets. We shall define as JFCs those with orbital periods P < 20 yr and Tisserand parameters in the range 2 < T K 3:1, while those comets coming from the same source, but that do not fulfill the previous criteria (mainly because they have periods P > 20 yr) will be called ‘non-JFCs’. We performed a series of numerical simulations of fictitious comets with a purely dynamical model and also with a more complete dynamical–physical model that includes besides nongravitational forces, sublimation and splitting mechanisms. With the dynamical model, we obtain a poor match between the computed distributions of orbital elements and the observed ones. However with the inclusion of physical effects in the complete model we are able to obtain good fits to observations. The best fits are attained with four splitting models with a relative weak dependence on q, and a mass loss in every splitting event that is less when the frequency is high and vice versa. The mean lifetime of JFCs with radii R > 1 km and q < 1:5 AU is found to be of about 150–200 revolutions (103 yrÞ. The total population of JFCs with radii R > 1 km within Jupiter’s zone is found to be of 450 50. Yet, the population of non-JFCs with radii R > 1 km in Jupiter-crossing orbits may be 4 times greater, thus leading to a whole population of JFCs + non-JFCs of 2250 250. Most of these comets have perihelia close to Jupiter’s orbit. On the other hand, very few non-JFCs reach the Earth’s vicinity (perihelion distances q K 2 AU) which gives additional support to the idea that JFCs and Halley-type comets have different dynamical origins. Our model allows us to define the zones of the orbital element space in which we would expect to find a large number of JFCs. This is the first time, to our knowledge, that a physicodynamical model is presented that includes sublimation and different splitting laws. Our work helps to understand the role played by these erosion effects in the distribution of the orbital elements and lifetimes of JFCs
Fil: Di Sisto, Romina Paula. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Fernández, Julio A.. Facultad de Ciencias; Uruguay
Fil: Brunini, Adrian. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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
Comets
Origins
Trans-Neptunian Objects
Dynamics
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:11336/42843

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network_name_str CONICET Digital (CONICET)
spelling On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulationsDi Sisto, Romina PaulaFernández, Julio A.Brunini, AdrianCometsOriginsTrans-Neptunian ObjectsDynamicshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We study the Jupiter family comet (JFC) population assumed to come from the Scattered Disk and transferred to the Jupiter’s zone through gravitational interactions with the Jovian planets. We shall define as JFCs those with orbital periods P < 20 yr and Tisserand parameters in the range 2 < T K 3:1, while those comets coming from the same source, but that do not fulfill the previous criteria (mainly because they have periods P > 20 yr) will be called ‘non-JFCs’. We performed a series of numerical simulations of fictitious comets with a purely dynamical model and also with a more complete dynamical–physical model that includes besides nongravitational forces, sublimation and splitting mechanisms. With the dynamical model, we obtain a poor match between the computed distributions of orbital elements and the observed ones. However with the inclusion of physical effects in the complete model we are able to obtain good fits to observations. The best fits are attained with four splitting models with a relative weak dependence on q, and a mass loss in every splitting event that is less when the frequency is high and vice versa. The mean lifetime of JFCs with radii R > 1 km and q < 1:5 AU is found to be of about 150–200 revolutions (103 yrÞ. The total population of JFCs with radii R > 1 km within Jupiter’s zone is found to be of 450 50. Yet, the population of non-JFCs with radii R > 1 km in Jupiter-crossing orbits may be 4 times greater, thus leading to a whole population of JFCs + non-JFCs of 2250 250. Most of these comets have perihelia close to Jupiter’s orbit. On the other hand, very few non-JFCs reach the Earth’s vicinity (perihelion distances q K 2 AU) which gives additional support to the idea that JFCs and Halley-type comets have different dynamical origins. Our model allows us to define the zones of the orbital element space in which we would expect to find a large number of JFCs. This is the first time, to our knowledge, that a physicodynamical model is presented that includes sublimation and different splitting laws. Our work helps to understand the role played by these erosion effects in the distribution of the orbital elements and lifetimes of JFCsFil: Di Sisto, Romina Paula. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Fernández, Julio A.. Facultad de Ciencias; UruguayFil: Brunini, Adrian. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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; ArgentinaAcademic Press Inc Elsevier Science2009-05info: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/11336/42843Di Sisto, Romina Paula; Fernández, Julio A.; Brunini, Adrian; On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations; Academic Press Inc Elsevier Science; Icarus; 203; 1; 5-2009; 140-1540019-1035CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1016/j.icarus.2009.05.002info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2009Icar..203..140Dinfo:eu-repo/semantics/altIdentifier/url/https://www.sciencedirect.com/science/article/pii/S0019103509001912?via%3Dihubinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:58:59Zoai:ri.conicet.gov.ar:11336/42843instacron: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 09:58:59.986CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations
title On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations
spellingShingle On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations
Di Sisto, Romina Paula
Comets
Origins
Trans-Neptunian Objects
Dynamics
title_short On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations
title_full On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations
title_fullStr On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations
title_full_unstemmed On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations
title_sort On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations
dc.creator.none.fl_str_mv Di Sisto, Romina Paula
Fernández, Julio A.
Brunini, Adrian
author Di Sisto, Romina Paula
author_facet Di Sisto, Romina Paula
Fernández, Julio A.
Brunini, Adrian
author_role author
author2 Fernández, Julio A.
Brunini, Adrian
author2_role author
author
dc.subject.none.fl_str_mv Comets
Origins
Trans-Neptunian Objects
Dynamics
topic Comets
Origins
Trans-Neptunian Objects
Dynamics
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We study the Jupiter family comet (JFC) population assumed to come from the Scattered Disk and transferred to the Jupiter’s zone through gravitational interactions with the Jovian planets. We shall define as JFCs those with orbital periods P < 20 yr and Tisserand parameters in the range 2 < T K 3:1, while those comets coming from the same source, but that do not fulfill the previous criteria (mainly because they have periods P > 20 yr) will be called ‘non-JFCs’. We performed a series of numerical simulations of fictitious comets with a purely dynamical model and also with a more complete dynamical–physical model that includes besides nongravitational forces, sublimation and splitting mechanisms. With the dynamical model, we obtain a poor match between the computed distributions of orbital elements and the observed ones. However with the inclusion of physical effects in the complete model we are able to obtain good fits to observations. The best fits are attained with four splitting models with a relative weak dependence on q, and a mass loss in every splitting event that is less when the frequency is high and vice versa. The mean lifetime of JFCs with radii R > 1 km and q < 1:5 AU is found to be of about 150–200 revolutions (103 yrÞ. The total population of JFCs with radii R > 1 km within Jupiter’s zone is found to be of 450 50. Yet, the population of non-JFCs with radii R > 1 km in Jupiter-crossing orbits may be 4 times greater, thus leading to a whole population of JFCs + non-JFCs of 2250 250. Most of these comets have perihelia close to Jupiter’s orbit. On the other hand, very few non-JFCs reach the Earth’s vicinity (perihelion distances q K 2 AU) which gives additional support to the idea that JFCs and Halley-type comets have different dynamical origins. Our model allows us to define the zones of the orbital element space in which we would expect to find a large number of JFCs. This is the first time, to our knowledge, that a physicodynamical model is presented that includes sublimation and different splitting laws. Our work helps to understand the role played by these erosion effects in the distribution of the orbital elements and lifetimes of JFCs
Fil: Di Sisto, Romina Paula. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Fernández, Julio A.. Facultad de Ciencias; Uruguay
Fil: Brunini, Adrian. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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 We study the Jupiter family comet (JFC) population assumed to come from the Scattered Disk and transferred to the Jupiter’s zone through gravitational interactions with the Jovian planets. We shall define as JFCs those with orbital periods P < 20 yr and Tisserand parameters in the range 2 < T K 3:1, while those comets coming from the same source, but that do not fulfill the previous criteria (mainly because they have periods P > 20 yr) will be called ‘non-JFCs’. We performed a series of numerical simulations of fictitious comets with a purely dynamical model and also with a more complete dynamical–physical model that includes besides nongravitational forces, sublimation and splitting mechanisms. With the dynamical model, we obtain a poor match between the computed distributions of orbital elements and the observed ones. However with the inclusion of physical effects in the complete model we are able to obtain good fits to observations. The best fits are attained with four splitting models with a relative weak dependence on q, and a mass loss in every splitting event that is less when the frequency is high and vice versa. The mean lifetime of JFCs with radii R > 1 km and q < 1:5 AU is found to be of about 150–200 revolutions (103 yrÞ. The total population of JFCs with radii R > 1 km within Jupiter’s zone is found to be of 450 50. Yet, the population of non-JFCs with radii R > 1 km in Jupiter-crossing orbits may be 4 times greater, thus leading to a whole population of JFCs + non-JFCs of 2250 250. Most of these comets have perihelia close to Jupiter’s orbit. On the other hand, very few non-JFCs reach the Earth’s vicinity (perihelion distances q K 2 AU) which gives additional support to the idea that JFCs and Halley-type comets have different dynamical origins. Our model allows us to define the zones of the orbital element space in which we would expect to find a large number of JFCs. This is the first time, to our knowledge, that a physicodynamical model is presented that includes sublimation and different splitting laws. Our work helps to understand the role played by these erosion effects in the distribution of the orbital elements and lifetimes of JFCs
publishDate 2009
dc.date.none.fl_str_mv 2009-05
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/11336/42843
Di Sisto, Romina Paula; Fernández, Julio A.; Brunini, Adrian; On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations; Academic Press Inc Elsevier Science; Icarus; 203; 1; 5-2009; 140-154
0019-1035
CONICET Digital
CONICET
url http://hdl.handle.net/11336/42843
identifier_str_mv Di Sisto, Romina Paula; Fernández, Julio A.; Brunini, Adrian; On the population, physical decay and orbital distribution of Jupiter family comets: Numerical simulations; Academic Press Inc Elsevier Science; Icarus; 203; 1; 5-2009; 140-154
0019-1035
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1016/j.icarus.2009.05.002
info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2009Icar..203..140D
info:eu-repo/semantics/altIdentifier/url/https://www.sciencedirect.com/science/article/pii/S0019103509001912?via%3Dihub
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
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
application/pdf
dc.publisher.none.fl_str_mv Academic Press Inc Elsevier Science
publisher.none.fl_str_mv Academic Press Inc Elsevier Science
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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