On the oldest asteroid families in the main belt

Página do item simplificado
dc.contributor.authorCarruba, V. [UNESP]
dc.contributor.authorNesvorný, D.
dc.contributor.authorAljbaae, S. [UNESP]
dc.contributor.authorDomingos, R. C. [UNESP]
dc.contributor.authorHuaman, M. [UNESP]
dc.contributor.institutionUniversidade Estadual Paulista (Unesp)
dc.contributor.institutionSouthwest Research Institute
dc.date.accessioned2018-12-11T17:28:06Z
dc.date.available2018-12-11T17:28:06Z
dc.date.issued2016-03-17
dc.description.abstractAsteroid families are groups of minor bodies produced by high-velocity collisions. After the initial dispersions of the parent bodies fragments, their orbits evolve because of several gravitational and non-gravitational effects, such as diffusion in mean-motion resonances, Yarkovsky and Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effects, close encounters of collisions, etc. The subsequent dynamical evolution of asteroid family members may cause some of the original fragments to travel beyond the conventional limits of the asteroid family. Eventually, the whole family will dynamically disperse and no longer be recognizable. A natural question that may arise concerns the time-scales for dispersion of large families. In particular, what is the oldest still recognizable family in the main belt? Are there any families that may date from the late stages of the late heavy bombardment and that could provide clues on our understanding of the primitive Solar system? In this work, we investigate the dynamical stability of seven of the allegedly oldest families in the asteroid main belt. Our results show that none of the seven studied families has a nominally mean estimated age older than 2.7 Gyr, assuming standard values for the parameters describing the strength of the Yarkovsky force. Most-paleo-families' that formed between 2.7 and 3.8 Gyr would be characterized by a very shallow size-frequency distribution, and could be recognizable only if located in a dynamically less active region (such as that of the Koronis family). V-type asteroids in the central main belt could be compatible with a formation from a paleo-Eunomia family.en
dc.description.affiliationUNESP - Univ. Estadual Paulista Grupo de dinâmica Orbital e Planetologia
dc.description.affiliationDepartment of Space Studies Southwest Research Institute
dc.description.affiliationUNESP - Univ. Estadual Paulista
dc.description.affiliationUnespUNESP - Univ. Estadual Paulista Grupo de dinâmica Orbital e Planetologia
dc.description.affiliationUnespUNESP - Univ. Estadual Paulista
dc.format.extent3731-3738
dc.identifierhttp://dx.doi.org/10.1093/mnras/stw533
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, v. 458, n. 4, p. 3731-3738, 2016.
dc.identifier.doi10.1093/mnras/stw533
dc.identifier.file2-s2.0-84965076181.pdf
dc.identifier.issn1365-2966
dc.identifier.issn0035-8711
dc.identifier.lattes6652169083464327
dc.identifier.orcid0000-0002-0516-0420
dc.identifier.scopus2-s2.0-84965076181
dc.identifier.urihttp://hdl.handle.net/11449/177998
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.relation.ispartofsjr2,346
dc.relation.ispartofsjr2,346
dc.rights.accessRightsAcesso aberto
dc.sourceScopus
dc.subjectCelestial mechanics
dc.subjectMinor planets, asteroids: General
dc.titleOn the oldest asteroid families in the main belten
dc.typeArtigo
unesp.author.lattes6652169083464327[4]
unesp.author.orcid0000-0002-0516-0420[4]

Arquivos

Pacote Original
Agora exibindo 1 - 1 de 1
Imagem de Miniatura
Nome:
2-s2.0-84965076181.pdf
Tamanho:
649.44 KB
Formato:
Adobe Portable Document Format
Descrição:
Baixar

Coleções

Artigos - Matemática - FEG