The population of rotational fission clusters inside asteroid collisional families
Autor(a) principal: | |
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Data de Publicação: | 2020 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1038/s41550-019-0887-8 http://hdl.handle.net/11449/201268 |
Resumo: | Asteroid families are groups of objects sharing similar orbits. They are mostly the results of past collisions between two asteroids. Recent studies have shown that some asteroid families can also be the outcome of the spin-up-induced fission of a critically rotating parent body (fission clusters). In at least four young fission clusters, more than 5% of their members belong to subfamilies, secondary clusters of objects mostly formed after the main fission event. However, asteroidal subfamilies are still not well characterized. In this work, using family recognition methods based on time-reversal dynamical simulations, machine-learning clustering algorithms and the exceptional orbit accuracy obtained from Gaia observations of Solar System objects, we identify several subclusters within four extremely young collisional families. We find that collisional asteroid families younger than 100 Myr have a higher fraction of young detectable fission subclusters with respect to older groups. The collisional events that form asteroid families may trigger a subsequent cascade of spin-induced formations of fission clusters by producing fragments in highly rotating states. |
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Repositório Institucional da UNESP |
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The population of rotational fission clusters inside asteroid collisional familiesAsteroid families are groups of objects sharing similar orbits. They are mostly the results of past collisions between two asteroids. Recent studies have shown that some asteroid families can also be the outcome of the spin-up-induced fission of a critically rotating parent body (fission clusters). In at least four young fission clusters, more than 5% of their members belong to subfamilies, secondary clusters of objects mostly formed after the main fission event. However, asteroidal subfamilies are still not well characterized. In this work, using family recognition methods based on time-reversal dynamical simulations, machine-learning clustering algorithms and the exceptional orbit accuracy obtained from Gaia observations of Solar System objects, we identify several subclusters within four extremely young collisional families. We find that collisional asteroid families younger than 100 Myr have a higher fraction of young detectable fission subclusters with respect to older groups. The collisional events that form asteroid families may trigger a subsequent cascade of spin-induced formations of fission clusters by producing fragments in highly rotating states.São Paulo State University (UNESP) School of Natural Sciences and EngineeringUniversité de la Côte d’Azur Observatoire de la Côte d’Azur (CNRS) Laboratoire LagrangeNational Space Research Institute (INPE) Division of Space Mechanics and ControlFederal University of São Paulo (UNIFESP) Science and Technology InstituteSão Paulo State University (UNESP) School of Natural Sciences and EngineeringUniversidade Estadual Paulista (Unesp)Laboratoire LagrangeDivision of Space Mechanics and ControlUniversidade de São Paulo (USP)Carruba, V. [UNESP]Spoto, F.Barletta, W. [UNESP]Aljbaae, S.Fazenda, L.Martins, B. [UNESP]2020-12-12T02:28:17Z2020-12-12T02:28:17Z2020-01-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article83-88http://dx.doi.org/10.1038/s41550-019-0887-8Nature Astronomy, v. 4, n. 1, p. 83-88, 2020.2397-3366http://hdl.handle.net/11449/20126810.1038/s41550-019-0887-82-s2.0-85073939909Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengNature Astronomyinfo:eu-repo/semantics/openAccess2024-07-02T14:28:52Zoai:repositorio.unesp.br:11449/201268Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-07-02T14:28:52Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
The population of rotational fission clusters inside asteroid collisional families |
title |
The population of rotational fission clusters inside asteroid collisional families |
spellingShingle |
The population of rotational fission clusters inside asteroid collisional families Carruba, V. [UNESP] |
title_short |
The population of rotational fission clusters inside asteroid collisional families |
title_full |
The population of rotational fission clusters inside asteroid collisional families |
title_fullStr |
The population of rotational fission clusters inside asteroid collisional families |
title_full_unstemmed |
The population of rotational fission clusters inside asteroid collisional families |
title_sort |
The population of rotational fission clusters inside asteroid collisional families |
author |
Carruba, V. [UNESP] |
author_facet |
Carruba, V. [UNESP] Spoto, F. Barletta, W. [UNESP] Aljbaae, S. Fazenda, L. Martins, B. [UNESP] |
author_role |
author |
author2 |
Spoto, F. Barletta, W. [UNESP] Aljbaae, S. Fazenda, L. Martins, B. [UNESP] |
author2_role |
author author author author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (Unesp) Laboratoire Lagrange Division of Space Mechanics and Control Universidade de São Paulo (USP) |
dc.contributor.author.fl_str_mv |
Carruba, V. [UNESP] Spoto, F. Barletta, W. [UNESP] Aljbaae, S. Fazenda, L. Martins, B. [UNESP] |
description |
Asteroid families are groups of objects sharing similar orbits. They are mostly the results of past collisions between two asteroids. Recent studies have shown that some asteroid families can also be the outcome of the spin-up-induced fission of a critically rotating parent body (fission clusters). In at least four young fission clusters, more than 5% of their members belong to subfamilies, secondary clusters of objects mostly formed after the main fission event. However, asteroidal subfamilies are still not well characterized. In this work, using family recognition methods based on time-reversal dynamical simulations, machine-learning clustering algorithms and the exceptional orbit accuracy obtained from Gaia observations of Solar System objects, we identify several subclusters within four extremely young collisional families. We find that collisional asteroid families younger than 100 Myr have a higher fraction of young detectable fission subclusters with respect to older groups. The collisional events that form asteroid families may trigger a subsequent cascade of spin-induced formations of fission clusters by producing fragments in highly rotating states. |
publishDate |
2020 |
dc.date.none.fl_str_mv |
2020-12-12T02:28:17Z 2020-12-12T02:28:17Z 2020-01-01 |
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/10.1038/s41550-019-0887-8 Nature Astronomy, v. 4, n. 1, p. 83-88, 2020. 2397-3366 http://hdl.handle.net/11449/201268 10.1038/s41550-019-0887-8 2-s2.0-85073939909 |
url |
http://dx.doi.org/10.1038/s41550-019-0887-8 http://hdl.handle.net/11449/201268 |
identifier_str_mv |
Nature Astronomy, v. 4, n. 1, p. 83-88, 2020. 2397-3366 10.1038/s41550-019-0887-8 2-s2.0-85073939909 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Nature Astronomy |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
83-88 |
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 |
|
_version_ |
1803649454267432960 |