Collisional study of Hilda and quasi-Hilda asteroids

Autores
Zain, Patricio Salvador; Di Sisto, Romina Paula; Gil-hutton, Ricardo Alfredo
Año de publicación
2025
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The Hilda asteroids are located in the outer main belt (MB) in a stable 3:2 mean-motion resonance (MMR) with Jupiter,while the quasi-Hildas have similar orbits but are not directly under the effect of the MMR. Moreover, cometary activity has beendetected in quasi-Hildas.Aims. In this study, we aim to investigate the collisional evolution of Hilda asteroids and apply it to an investigation into the cratering onasteroid (334) Chicago; we also intend to determine whether impacts between Hildas and quasi-Hildas can serve as a viable mechanismfor inducing cometary activity.Methods. Using the Asteroid Collisions and Dynamic Computation (ACDC) code, we simulated the collisional evolution of Hildaasteroids over a period of 4 Gyr. We considered three initial size-frequency distributions (SFDs) and two scaling laws for the collisionaloutcomes and performed a large set of simulations for each scenario, which we used to construct median SFDs of the Hilda population.We also derived an impactor SFD on asteroid (334) Chicago and used it to calculate the crater SFD on (334) Chicago. Additionally,we evaluated the sub-catastrophic impact timescale between Hilda and quasi-Hilda objects.Results. The observed SFD of Hilda asteroids larger than 3 km is best matched by scenarios assuming that such an SFD is mostlyprimordial, implying minimal collisional activity over time. For smaller sizes, although unconstrained, the SFD steepens significantlydue to the catastrophic fragmentation of a small number of multi-kilometre-sized bodies. We determined that the largest impactor on(334) Chicago measures a few kilometres in size, resulting in a maximum crater size of approximately 30 km. Furthermore, the slopeof the crater SFD mirrors that of the initial SFD for sub-kilometric bodies. While impact events between Hildas and quasi-Hildascan induce observable activity, and although it is stochastic in nature, the timescale of such events exceeds the dynamical lifetime ofquasi-Hildas, making them an unlikely primary mechanism for inducing observable activity.
Fil: Zain, Patricio Salvador. 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: Di Sisto, Romina Paula. 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Gil-hutton, Ricardo Alfredo. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan; Argentina
Materia
NUMERICAL
STATISTICAL
ASTEROIDS
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:11336/290808
Acceder
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network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling Collisional study of Hilda and quasi-Hilda asteroidsZain, Patricio SalvadorDi Sisto, Romina PaulaGil-hutton, Ricardo AlfredoNUMERICALSTATISTICALASTEROIDShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The Hilda asteroids are located in the outer main belt (MB) in a stable 3:2 mean-motion resonance (MMR) with Jupiter,while the quasi-Hildas have similar orbits but are not directly under the effect of the MMR. Moreover, cometary activity has beendetected in quasi-Hildas.Aims. In this study, we aim to investigate the collisional evolution of Hilda asteroids and apply it to an investigation into the cratering onasteroid (334) Chicago; we also intend to determine whether impacts between Hildas and quasi-Hildas can serve as a viable mechanismfor inducing cometary activity.Methods. Using the Asteroid Collisions and Dynamic Computation (ACDC) code, we simulated the collisional evolution of Hildaasteroids over a period of 4 Gyr. We considered three initial size-frequency distributions (SFDs) and two scaling laws for the collisionaloutcomes and performed a large set of simulations for each scenario, which we used to construct median SFDs of the Hilda population.We also derived an impactor SFD on asteroid (334) Chicago and used it to calculate the crater SFD on (334) Chicago. Additionally,we evaluated the sub-catastrophic impact timescale between Hilda and quasi-Hilda objects.Results. The observed SFD of Hilda asteroids larger than 3 km is best matched by scenarios assuming that such an SFD is mostlyprimordial, implying minimal collisional activity over time. For smaller sizes, although unconstrained, the SFD steepens significantlydue to the catastrophic fragmentation of a small number of multi-kilometre-sized bodies. We determined that the largest impactor on(334) Chicago measures a few kilometres in size, resulting in a maximum crater size of approximately 30 km. Furthermore, the slopeof the crater SFD mirrors that of the initial SFD for sub-kilometric bodies. While impact events between Hildas and quasi-Hildascan induce observable activity, and although it is stochastic in nature, the timescale of such events exceeds the dynamical lifetime ofquasi-Hildas, making them an unlikely primary mechanism for inducing observable activity.Fil: Zain, Patricio Salvador. 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: Di Sisto, Romina Paula. 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Gil-hutton, Ricardo Alfredo. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan; ArgentinaEDP Sciences2025-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/290808Zain, Patricio Salvador; Di Sisto, Romina Paula; Gil-hutton, Ricardo Alfredo; Collisional study of Hilda and quasi-Hilda asteroids; EDP Sciences; Astronomy and Astrophysics; 694; 2-2025; 1-80004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202450850info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450850info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-08-25T15:46:34Zoai:ri.conicet.gov.ar:11336/290808instacron: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:34982026-08-25 15:46:34.602CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Collisional study of Hilda and quasi-Hilda asteroids
title Collisional study of Hilda and quasi-Hilda asteroids
spellingShingle Collisional study of Hilda and quasi-Hilda asteroids
Zain, Patricio Salvador
NUMERICAL
STATISTICAL
ASTEROIDS
title_short Collisional study of Hilda and quasi-Hilda asteroids
title_full Collisional study of Hilda and quasi-Hilda asteroids
title_fullStr Collisional study of Hilda and quasi-Hilda asteroids
title_full_unstemmed Collisional study of Hilda and quasi-Hilda asteroids
title_sort Collisional study of Hilda and quasi-Hilda asteroids
dc.creator.none.fl_str_mv Zain, Patricio Salvador
Di Sisto, Romina Paula
Gil-hutton, Ricardo Alfredo
author Zain, Patricio Salvador
author_facet Zain, Patricio Salvador
Di Sisto, Romina Paula
Gil-hutton, Ricardo Alfredo
author_role author
author2 Di Sisto, Romina Paula
Gil-hutton, Ricardo Alfredo
author2_role author
author
dc.subject.none.fl_str_mv NUMERICAL
STATISTICAL
ASTEROIDS
topic NUMERICAL
STATISTICAL
ASTEROIDS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. The Hilda asteroids are located in the outer main belt (MB) in a stable 3:2 mean-motion resonance (MMR) with Jupiter,while the quasi-Hildas have similar orbits but are not directly under the effect of the MMR. Moreover, cometary activity has beendetected in quasi-Hildas.Aims. In this study, we aim to investigate the collisional evolution of Hilda asteroids and apply it to an investigation into the cratering onasteroid (334) Chicago; we also intend to determine whether impacts between Hildas and quasi-Hildas can serve as a viable mechanismfor inducing cometary activity.Methods. Using the Asteroid Collisions and Dynamic Computation (ACDC) code, we simulated the collisional evolution of Hildaasteroids over a period of 4 Gyr. We considered three initial size-frequency distributions (SFDs) and two scaling laws for the collisionaloutcomes and performed a large set of simulations for each scenario, which we used to construct median SFDs of the Hilda population.We also derived an impactor SFD on asteroid (334) Chicago and used it to calculate the crater SFD on (334) Chicago. Additionally,we evaluated the sub-catastrophic impact timescale between Hilda and quasi-Hilda objects.Results. The observed SFD of Hilda asteroids larger than 3 km is best matched by scenarios assuming that such an SFD is mostlyprimordial, implying minimal collisional activity over time. For smaller sizes, although unconstrained, the SFD steepens significantlydue to the catastrophic fragmentation of a small number of multi-kilometre-sized bodies. We determined that the largest impactor on(334) Chicago measures a few kilometres in size, resulting in a maximum crater size of approximately 30 km. Furthermore, the slopeof the crater SFD mirrors that of the initial SFD for sub-kilometric bodies. While impact events between Hildas and quasi-Hildascan induce observable activity, and although it is stochastic in nature, the timescale of such events exceeds the dynamical lifetime ofquasi-Hildas, making them an unlikely primary mechanism for inducing observable activity.
Fil: Zain, Patricio Salvador. 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: Di Sisto, Romina Paula. 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Gil-hutton, Ricardo Alfredo. Universidad Nacional de San Juan. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Geofísica y Astronomía; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan; Argentina
description Context. The Hilda asteroids are located in the outer main belt (MB) in a stable 3:2 mean-motion resonance (MMR) with Jupiter,while the quasi-Hildas have similar orbits but are not directly under the effect of the MMR. Moreover, cometary activity has beendetected in quasi-Hildas.Aims. In this study, we aim to investigate the collisional evolution of Hilda asteroids and apply it to an investigation into the cratering onasteroid (334) Chicago; we also intend to determine whether impacts between Hildas and quasi-Hildas can serve as a viable mechanismfor inducing cometary activity.Methods. Using the Asteroid Collisions and Dynamic Computation (ACDC) code, we simulated the collisional evolution of Hildaasteroids over a period of 4 Gyr. We considered three initial size-frequency distributions (SFDs) and two scaling laws for the collisionaloutcomes and performed a large set of simulations for each scenario, which we used to construct median SFDs of the Hilda population.We also derived an impactor SFD on asteroid (334) Chicago and used it to calculate the crater SFD on (334) Chicago. Additionally,we evaluated the sub-catastrophic impact timescale between Hilda and quasi-Hilda objects.Results. The observed SFD of Hilda asteroids larger than 3 km is best matched by scenarios assuming that such an SFD is mostlyprimordial, implying minimal collisional activity over time. For smaller sizes, although unconstrained, the SFD steepens significantlydue to the catastrophic fragmentation of a small number of multi-kilometre-sized bodies. We determined that the largest impactor on(334) Chicago measures a few kilometres in size, resulting in a maximum crater size of approximately 30 km. Furthermore, the slopeof the crater SFD mirrors that of the initial SFD for sub-kilometric bodies. While impact events between Hildas and quasi-Hildascan induce observable activity, and although it is stochastic in nature, the timescale of such events exceeds the dynamical lifetime ofquasi-Hildas, making them an unlikely primary mechanism for inducing observable activity.
publishDate 2025
dc.date.none.fl_str_mv 2025-02
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/11336/290808
Zain, Patricio Salvador; Di Sisto, Romina Paula; Gil-hutton, Ricardo Alfredo; Collisional study of Hilda and quasi-Hilda asteroids; EDP Sciences; Astronomy and Astrophysics; 694; 2-2025; 1-8
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/290808
identifier_str_mv Zain, Patricio Salvador; Di Sisto, Romina Paula; Gil-hutton, Ricardo Alfredo; Collisional study of Hilda and quasi-Hilda asteroids; EDP Sciences; Astronomy and Astrophysics; 694; 2-2025; 1-8
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/url/https://www.aanda.org/10.1051/0004-6361/202450850
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450850
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
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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
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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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