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

Autores
Di Sisto, Romina Paula; Fernández, Julio A.; Brunini, Adrián
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<20yr and Tisserand parameters in the range 220yr) 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>1km and q<1.5AU is found to be of about 150-200 revolutions (˜103yr). The total population of JFCs with radii R>1km within Jupiter’s zone is found to be of 450±50. Yet, the population of non-JFCs with radii R>1km 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≲2AU) 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 physico-dynamical 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.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
Comets, dynamics
Comets, origin
Trans-neptunian objects
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/2089

id SEDICI_327011718cbf608dae884f5e2310d069
oai_identifier_str oai:sedici.unlp.edu.ar:10915/2089
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling On the population, physical decay and orbital distribution of Jupiter family comets: numerical simulationsDi Sisto, Romina PaulaFernández, Julio A.Brunini, AdriánCiencias AstronómicasComets, dynamicsComets, originTrans-neptunian objectsWe 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<20yr and Tisserand parameters in the range 2<T≲3.1, while those comets coming from the same source, but that do not fulfill the previous criteria (mainly because they have periods P>20yr) 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>1km and q<1.5AU is found to be of about 150-200 revolutions (˜10<SUP>3</SUP>yr). The total population of JFCs with radii R>1km within Jupiter’s zone is found to be of 450±50. Yet, the population of non-JFCs with radii R>1km 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≲2AU) 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 physico-dynamical 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.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2009info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf140-154http://sedici.unlp.edu.ar/handle/10915/2089enginfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2009Icar..203..140Dinfo:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0019103509001912#info:eu-repo/semantics/altIdentifier/issn/0019-1035info:eu-repo/semantics/altIdentifier/doi/10.1016/j.icarus.2009.05.002info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T10:48:37Zoai:sedici.unlp.edu.ar:10915/2089Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 10:48:39.103SEDICI (UNLP) - Universidad Nacional de La Platafalse
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
Ciencias Astronómicas
Comets, dynamics
Comets, origin
Trans-neptunian objects
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, Adrián
author Di Sisto, Romina Paula
author_facet Di Sisto, Romina Paula
Fernández, Julio A.
Brunini, Adrián
author_role author
author2 Fernández, Julio A.
Brunini, Adrián
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Comets, dynamics
Comets, origin
Trans-neptunian objects
topic Ciencias Astronómicas
Comets, dynamics
Comets, origin
Trans-neptunian objects
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<20yr and Tisserand parameters in the range 2<T≲3.1, while those comets coming from the same source, but that do not fulfill the previous criteria (mainly because they have periods P>20yr) 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>1km and q<1.5AU is found to be of about 150-200 revolutions (˜10<SUP>3</SUP>yr). The total population of JFCs with radii R>1km within Jupiter’s zone is found to be of 450±50. Yet, the population of non-JFCs with radii R>1km 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≲2AU) 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 physico-dynamical 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.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
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<20yr and Tisserand parameters in the range 2<T≲3.1, while those comets coming from the same source, but that do not fulfill the previous criteria (mainly because they have periods P>20yr) 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>1km and q<1.5AU is found to be of about 150-200 revolutions (˜10<SUP>3</SUP>yr). The total population of JFCs with radii R>1km within Jupiter’s zone is found to be of 450±50. Yet, the population of non-JFCs with radii R>1km 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≲2AU) 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 physico-dynamical 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
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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://sedici.unlp.edu.ar/handle/10915/2089
url http://sedici.unlp.edu.ar/handle/10915/2089
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2009Icar..203..140D
info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0019103509001912#
info:eu-repo/semantics/altIdentifier/issn/0019-1035
info:eu-repo/semantics/altIdentifier/doi/10.1016/j.icarus.2009.05.002
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
dc.format.none.fl_str_mv application/pdf
140-154
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
_version_ 1844615739257913344
score 13.070432