Cratering rate on Pluto produced by the inner trans-Neptunian population

Autores
Calandra, Maria Florencia; Gil Hutton, Ricardo Alfredo
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. The aim of this work is to obtain the cratering rate on Pluto and to estimate the size distribution of the population in the inner trans-Neptunian region. Methods. We find the intrinsic collisional probability and the mean collision velocity for the interaction between Pluto and the projectile population crossing its orbit, using the L7 Synthetic Model from the CFEPS Project. The size distribution of this population is found using the smallest satellite of Pluto, Styx, as a constraint, because it survives the collisional process for the solar system age. Results. We find that the mean intrinsic collisional probability and mean collision velocity between Pluto and the projectile population are (Pi) = 1.3098 × 10-22 km-2 yr-1 and (Vcol) = 2.005 ± 0.822 km s-1. If the projectile sample is separated between Plutinos and non-Plutinos and the intrinsic collisional probability of these sub-populations are taken into account, we find a ratio of approximately 20:1 in favor of non-Plutinos resulting in the greatest contribution to the cratering rate on Pluto. The projectile population for the inner trans-Neptunian belt is characterized using a double power-law mean-size distribution with exponents qA = 3.5 and qB = 5.14 for the small and large size end of the population, respectively, and break radius at rb = 11.86 km or 7.25 km for mean densities of the projectiles ρ1 = 1.85 g cm-3 and ρ2 = 1 g cm-3. With this mean-size distribution we find that an object with radius of ~28 km produces a crater in Pluto with a diameter of ~250 km in a time larger than the solar system age, indicating that this kind of large structure has a very low probability of occurrence.
Fil: Calandra, Maria Florencia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Casleo Sede San Juan; Argentina
Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Casleo Sede San Juan; Argentina. Universidad Nacional de San Juan; Argentina
Materia
KUIPER BELT: GENERAL
METHODS: NUMERICAL
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:11336/63630
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/63630
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Cratering rate on Pluto produced by the inner trans-Neptunian populationCalandra, Maria FlorenciaGil Hutton, Ricardo AlfredoKUIPER BELT: GENERALMETHODS: NUMERICALPLANETS AND SATELLITES: GENERALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. The aim of this work is to obtain the cratering rate on Pluto and to estimate the size distribution of the population in the inner trans-Neptunian region. Methods. We find the intrinsic collisional probability and the mean collision velocity for the interaction between Pluto and the projectile population crossing its orbit, using the L7 Synthetic Model from the CFEPS Project. The size distribution of this population is found using the smallest satellite of Pluto, Styx, as a constraint, because it survives the collisional process for the solar system age. Results. We find that the mean intrinsic collisional probability and mean collision velocity between Pluto and the projectile population are (Pi) = 1.3098 × 10-22 km-2 yr-1 and (Vcol) = 2.005 ± 0.822 km s-1. If the projectile sample is separated between Plutinos and non-Plutinos and the intrinsic collisional probability of these sub-populations are taken into account, we find a ratio of approximately 20:1 in favor of non-Plutinos resulting in the greatest contribution to the cratering rate on Pluto. The projectile population for the inner trans-Neptunian belt is characterized using a double power-law mean-size distribution with exponents qA = 3.5 and qB = 5.14 for the small and large size end of the population, respectively, and break radius at rb = 11.86 km or 7.25 km for mean densities of the projectiles ρ1 = 1.85 g cm-3 and ρ2 = 1 g cm-3. With this mean-size distribution we find that an object with radius of ~28 km produces a crater in Pluto with a diameter of ~250 km in a time larger than the solar system age, indicating that this kind of large structure has a very low probability of occurrence.Fil: Calandra, Maria Florencia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Casleo Sede San Juan; ArgentinaFil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Casleo Sede San Juan; Argentina. Universidad Nacional de San Juan; ArgentinaEDP Sciences2017-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/63630Calandra, Maria Florencia; Gil Hutton, Ricardo Alfredo; Cratering rate on Pluto produced by the inner trans-Neptunian population; EDP Sciences; Astronomy and Astrophysics; 601; a116; 5-2017; 1-50004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628930info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/05/aa28930-16/aa28930-16.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:21:08Zoai:ri.conicet.gov.ar:11336/63630instacron: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:34982025-10-22 11:21:08.639CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Cratering rate on Pluto produced by the inner trans-Neptunian population
title Cratering rate on Pluto produced by the inner trans-Neptunian population
spellingShingle Cratering rate on Pluto produced by the inner trans-Neptunian population
Calandra, Maria Florencia
KUIPER BELT: GENERAL
METHODS: NUMERICAL
PLANETS AND SATELLITES: GENERAL
title_short Cratering rate on Pluto produced by the inner trans-Neptunian population
title_full Cratering rate on Pluto produced by the inner trans-Neptunian population
title_fullStr Cratering rate on Pluto produced by the inner trans-Neptunian population
title_full_unstemmed Cratering rate on Pluto produced by the inner trans-Neptunian population
title_sort Cratering rate on Pluto produced by the inner trans-Neptunian population
dc.creator.none.fl_str_mv Calandra, Maria Florencia
Gil Hutton, Ricardo Alfredo
author Calandra, Maria Florencia
author_facet Calandra, Maria Florencia
Gil Hutton, Ricardo Alfredo
author_role author
author2 Gil Hutton, Ricardo Alfredo
author2_role author
dc.subject.none.fl_str_mv KUIPER BELT: GENERAL
METHODS: NUMERICAL
PLANETS AND SATELLITES: GENERAL
topic KUIPER BELT: GENERAL
METHODS: NUMERICAL
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 Aims. The aim of this work is to obtain the cratering rate on Pluto and to estimate the size distribution of the population in the inner trans-Neptunian region. Methods. We find the intrinsic collisional probability and the mean collision velocity for the interaction between Pluto and the projectile population crossing its orbit, using the L7 Synthetic Model from the CFEPS Project. The size distribution of this population is found using the smallest satellite of Pluto, Styx, as a constraint, because it survives the collisional process for the solar system age. Results. We find that the mean intrinsic collisional probability and mean collision velocity between Pluto and the projectile population are (Pi) = 1.3098 × 10-22 km-2 yr-1 and (Vcol) = 2.005 ± 0.822 km s-1. If the projectile sample is separated between Plutinos and non-Plutinos and the intrinsic collisional probability of these sub-populations are taken into account, we find a ratio of approximately 20:1 in favor of non-Plutinos resulting in the greatest contribution to the cratering rate on Pluto. The projectile population for the inner trans-Neptunian belt is characterized using a double power-law mean-size distribution with exponents qA = 3.5 and qB = 5.14 for the small and large size end of the population, respectively, and break radius at rb = 11.86 km or 7.25 km for mean densities of the projectiles ρ1 = 1.85 g cm-3 and ρ2 = 1 g cm-3. With this mean-size distribution we find that an object with radius of ~28 km produces a crater in Pluto with a diameter of ~250 km in a time larger than the solar system age, indicating that this kind of large structure has a very low probability of occurrence.
Fil: Calandra, Maria Florencia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Casleo Sede San Juan; Argentina
Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de San Juan. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de la Plata. Complejo Astronómico "el Leoncito". Casleo Sede San Juan | Universidad Nacional de Córdoba. Complejo Astronómico "el Leoncito". Casleo Sede San Juan; Argentina. Universidad Nacional de San Juan; Argentina
description Aims. The aim of this work is to obtain the cratering rate on Pluto and to estimate the size distribution of the population in the inner trans-Neptunian region. Methods. We find the intrinsic collisional probability and the mean collision velocity for the interaction between Pluto and the projectile population crossing its orbit, using the L7 Synthetic Model from the CFEPS Project. The size distribution of this population is found using the smallest satellite of Pluto, Styx, as a constraint, because it survives the collisional process for the solar system age. Results. We find that the mean intrinsic collisional probability and mean collision velocity between Pluto and the projectile population are (Pi) = 1.3098 × 10-22 km-2 yr-1 and (Vcol) = 2.005 ± 0.822 km s-1. If the projectile sample is separated between Plutinos and non-Plutinos and the intrinsic collisional probability of these sub-populations are taken into account, we find a ratio of approximately 20:1 in favor of non-Plutinos resulting in the greatest contribution to the cratering rate on Pluto. The projectile population for the inner trans-Neptunian belt is characterized using a double power-law mean-size distribution with exponents qA = 3.5 and qB = 5.14 for the small and large size end of the population, respectively, and break radius at rb = 11.86 km or 7.25 km for mean densities of the projectiles ρ1 = 1.85 g cm-3 and ρ2 = 1 g cm-3. With this mean-size distribution we find that an object with radius of ~28 km produces a crater in Pluto with a diameter of ~250 km in a time larger than the solar system age, indicating that this kind of large structure has a very low probability of occurrence.
publishDate 2017
dc.date.none.fl_str_mv 2017-05
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/11336/63630
Calandra, Maria Florencia; Gil Hutton, Ricardo Alfredo; Cratering rate on Pluto produced by the inner trans-Neptunian population; EDP Sciences; Astronomy and Astrophysics; 601; a116; 5-2017; 1-5
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/63630
identifier_str_mv Calandra, Maria Florencia; Gil Hutton, Ricardo Alfredo; Cratering rate on Pluto produced by the inner trans-Neptunian population; EDP Sciences; Astronomy and Astrophysics; 601; a116; 5-2017; 1-5
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628930
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/05/aa28930-16/aa28930-16.html
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
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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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score 12.982451

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