Constraints on the original ejection velocity fields of asteroid families

Detalhes bibliográficos
Autor(a) principal: Carruba, V. [UNESP]
Data de Publicação: 2016
Outros Autores: Nesvorný, D.
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UNESP
Texto Completo: http://dx.doi.org/10.1093/mnras/stw043
http://hdl.handle.net/11449/177952
Resumo: Asteroid families form as a result of large-scale collisions among main belt asteroids. The orbital distribution of fragments after a family-forming impact could inform us about their ejection velocities. Unfortunately, however, orbits dynamically evolve by a number of effects, including the Yarkovsky drift, chaotic diffusion, and gravitational encounters with massive asteroids, such that it is difficult to infer the ejection velocities eons after each family's formation. Here, we analyse the inclination distribution of asteroid families, because proper inclination can remain constant over long time intervals, and could help us to understand the distribution of the component of the ejection velocity that is perpendicular to the orbital plane (υW). From modelling the initial break up, we find that the distribution of υW of the fragments, which manage to escape the parent body's gravity, should be more peaked than a Gaussian distribution (i.e. be leptokurtic) even if the initial distribution was Gaussian. We surveyed known asteroid families for signs of a peaked distribution of υW using a statistical measure of the distribution peakedness or flatness known as kurtosis. We identified eight families whose υW distribution is significantly leptokurtic. These cases (e.g. the Koronis family) are located in dynamically quiet regions of themain belt, where, presumably, the initial distribution of υW was not modified by subsequent orbital evolution. We suggest that, in these cases, the inclination distribution can be used to obtain interesting information about the original ejection velocity field.
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spelling Constraints on the original ejection velocity fields of asteroid familiesAsteroids: generalCelestial mechanicsMinor planetsAsteroid families form as a result of large-scale collisions among main belt asteroids. The orbital distribution of fragments after a family-forming impact could inform us about their ejection velocities. Unfortunately, however, orbits dynamically evolve by a number of effects, including the Yarkovsky drift, chaotic diffusion, and gravitational encounters with massive asteroids, such that it is difficult to infer the ejection velocities eons after each family's formation. Here, we analyse the inclination distribution of asteroid families, because proper inclination can remain constant over long time intervals, and could help us to understand the distribution of the component of the ejection velocity that is perpendicular to the orbital plane (υW). From modelling the initial break up, we find that the distribution of υW of the fragments, which manage to escape the parent body's gravity, should be more peaked than a Gaussian distribution (i.e. be leptokurtic) even if the initial distribution was Gaussian. We surveyed known asteroid families for signs of a peaked distribution of υW using a statistical measure of the distribution peakedness or flatness known as kurtosis. We identified eight families whose υW distribution is significantly leptokurtic. These cases (e.g. the Koronis family) are located in dynamically quiet regions of themain belt, where, presumably, the initial distribution of υW was not modified by subsequent orbital evolution. We suggest that, in these cases, the inclination distribution can be used to obtain interesting information about the original ejection velocity field.National Science FoundationDepartment of Space Studies Southwest Research InstituteUNESP Univ. Estadual Paulista Grupo de dinâmica Orbital e PlanetologiaUNESP Univ. Estadual Paulista Grupo de dinâmica Orbital e PlanetologiaSouthwest Research InstituteUniversidade Estadual Paulista (Unesp)Carruba, V. [UNESP]Nesvorný, D.2018-12-11T17:27:50Z2018-12-11T17:27:50Z2016-04-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article1332-1338application/pdfhttp://dx.doi.org/10.1093/mnras/stw043Monthly Notices of the Royal Astronomical Society, v. 457, n. 2, p. 1332-1338, 2016.1365-29660035-8711http://hdl.handle.net/11449/17795210.1093/mnras/stw0432-s2.0-849636161592-s2.0-84963616159.pdfScopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Society2,3462,346info:eu-repo/semantics/openAccess2024-07-02T14:29:32Zoai:repositorio.unesp.br:11449/177952Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T23:28:40.688610Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false
dc.title.none.fl_str_mv Constraints on the original ejection velocity fields of asteroid families
title Constraints on the original ejection velocity fields of asteroid families
spellingShingle Constraints on the original ejection velocity fields of asteroid families
Carruba, V. [UNESP]
Asteroids: general
Celestial mechanics
Minor planets
title_short Constraints on the original ejection velocity fields of asteroid families
title_full Constraints on the original ejection velocity fields of asteroid families
title_fullStr Constraints on the original ejection velocity fields of asteroid families
title_full_unstemmed Constraints on the original ejection velocity fields of asteroid families
title_sort Constraints on the original ejection velocity fields of asteroid families
author Carruba, V. [UNESP]
author_facet Carruba, V. [UNESP]
Nesvorný, D.
author_role author
author2 Nesvorný, D.
author2_role author
dc.contributor.none.fl_str_mv Southwest Research Institute
Universidade Estadual Paulista (Unesp)
dc.contributor.author.fl_str_mv Carruba, V. [UNESP]
Nesvorný, D.
dc.subject.por.fl_str_mv Asteroids: general
Celestial mechanics
Minor planets
topic Asteroids: general
Celestial mechanics
Minor planets
description Asteroid families form as a result of large-scale collisions among main belt asteroids. The orbital distribution of fragments after a family-forming impact could inform us about their ejection velocities. Unfortunately, however, orbits dynamically evolve by a number of effects, including the Yarkovsky drift, chaotic diffusion, and gravitational encounters with massive asteroids, such that it is difficult to infer the ejection velocities eons after each family's formation. Here, we analyse the inclination distribution of asteroid families, because proper inclination can remain constant over long time intervals, and could help us to understand the distribution of the component of the ejection velocity that is perpendicular to the orbital plane (υW). From modelling the initial break up, we find that the distribution of υW of the fragments, which manage to escape the parent body's gravity, should be more peaked than a Gaussian distribution (i.e. be leptokurtic) even if the initial distribution was Gaussian. We surveyed known asteroid families for signs of a peaked distribution of υW using a statistical measure of the distribution peakedness or flatness known as kurtosis. We identified eight families whose υW distribution is significantly leptokurtic. These cases (e.g. the Koronis family) are located in dynamically quiet regions of themain belt, where, presumably, the initial distribution of υW was not modified by subsequent orbital evolution. We suggest that, in these cases, the inclination distribution can be used to obtain interesting information about the original ejection velocity field.
publishDate 2016
dc.date.none.fl_str_mv 2016-04-01
2018-12-11T17:27:50Z
2018-12-11T17:27:50Z
dc.type.status.fl_str_mv info:eu-repo/semantics/publishedVersion
dc.type.driver.fl_str_mv info:eu-repo/semantics/article
format article
status_str publishedVersion
dc.identifier.uri.fl_str_mv http://dx.doi.org/10.1093/mnras/stw043
Monthly Notices of the Royal Astronomical Society, v. 457, n. 2, p. 1332-1338, 2016.
1365-2966
0035-8711
http://hdl.handle.net/11449/177952
10.1093/mnras/stw043
2-s2.0-84963616159
2-s2.0-84963616159.pdf
url http://dx.doi.org/10.1093/mnras/stw043
http://hdl.handle.net/11449/177952
identifier_str_mv Monthly Notices of the Royal Astronomical Society, v. 457, n. 2, p. 1332-1338, 2016.
1365-2966
0035-8711
10.1093/mnras/stw043
2-s2.0-84963616159
2-s2.0-84963616159.pdf
dc.language.iso.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv Monthly Notices of the Royal Astronomical Society
2,346
2,346
dc.rights.driver.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv 1332-1338
application/pdf
dc.source.none.fl_str_mv Scopus
reponame:Repositório Institucional da UNESP
instname:Universidade Estadual Paulista (UNESP)
instacron:UNESP
instname_str Universidade Estadual Paulista (UNESP)
instacron_str UNESP
institution UNESP
reponame_str Repositório Institucional da UNESP
collection Repositório Institucional da UNESP
repository.name.fl_str_mv Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)
repository.mail.fl_str_mv
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