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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/42843
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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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1844613753781354496 |
score |
13.070432 |