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2 referências encontradas buscando em 15 dentre 15 sites.
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Área de identificação
Tipo de ReferênciaJournal Article
Sitemtc-m21b.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP5W34M/3FA7RGQ
Repositóriosid.inpe.br/mtc-m21b/2013/11.27.13.23.10
Última Atualização2014:01.20.15.44.22 administrator
Metadadossid.inpe.br/mtc-m21b/2013/11.27.13.23.11
Última Atualização dos Metadados2018:06.04.03.14.16 administrator
DOI10.1093/mnras/stt884
ISSN0035-8711
Rótuloisi 2013-11
Chave de CitaçãoCarrubaDoNeRoHuSo:2013:MuApAs
TítuloA multidomain approach to asteroid families' identification
Ano2013
MêsAug.
Data de Acesso24 fev. 2021
Número de Arquivos1
Tamanho3643 KiB
Área de contextualização
Autor1 Carruba, V.
2 Domingos, Rita de Cássia
3 Nesvorny, D.
4 Roig, F.
5 Huaman, M. E.
6 Souami, D.
Grupo1
2 ETE-ETE-INPE-MCTI-GOV-BR
Afiliação1 Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, Brazil.
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 SWRI, Boulder, CO 80302 USA.
4 ON, BR-20921400 Rio De Janeiro, RJ, Brazil.
5 Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, Brazil.
6 Univ Paris 06, F-75005 Paris, France.; UPMC, Observ Paris, SYRTE, CNRS UMR 8630, F-75014 Paris, France.
Endereço de e-Mailmarcelo.pazos@inpe.br
RevistaMonthly Notices of the Royal Astronomical Society
Volume433
Número3
Páginas2075-2096
Tipo SecundárioPRE PI
Nota SecundáriaA1 A1 A1 A2 A2 A2 B3 C
Histórico2018-06-04 03:14:16 :: administrator -> marcelo.pazos@inpe.br :: 2013
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãofinaldraft
Palavras-ChaveCelestial mechanics, minor planets, asteroids: general.
ResumoIt has been shown that large families are not limited to what found by hierarchical clustering methods in the domain of proper elements (a, e, sin(i)), which seems to be biased to find compact, relatively young clusters, but that there exists an extended population of objects with similar taxonomy and geometric albedo, which can extend to much larger regions in proper elements and frequencies domains: the family `halo'. Numerical simulations can be used to provide estimates of the age of the family halo, which can then be compared with ages of the family obtained with other methods. Determining a good estimate of the possible orbital extension of a family halo is therefore quite important, if one is interested in determining its age and, possibly, the original ejection velocity field. Previous works have identified families' haloes by an analysis in proper elements domains, or by using Sloan Digital Sky Survey-Moving Object Catalog data, fourth release (SDSS-MOC4) multiband photometry to infer the asteroid taxonomy, or by a combination of the two methods. The limited number of asteroids for which geometric albedo was known until recently discouraged in the past the extensive use of this additional parameter, which is however of great importance in identifying an asteroid taxonomy. The new availability of geometric albedo data from the Wide-field Infrared Survey Explorer (WISE) mission for about 100 000 asteroids significantly increased the sample of objects for which such information, with some errors, is now known. In this work, we proposed a new method to identify families' haloes in a multidomain space composed by proper elements, SDSS-MOC4 (a*, i - z) colours, and WISE geometric albedo for the whole main belt (and the Hungaria and Cybele orbital regions). Assuming that most families were created by the breakup of an undifferentiated parent body, they are expected to be homogeneous in colours and albedo. The new method is quite effective in determining objects belonging to a family halo, with low percentages of likely interlopers, and results that are quite consistent in term of taxonomy and geometric albedo of the halo members.
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Repositório Espelhoiconet.com.br/banon/2006/11.26.21.31
Unidades Imediatamente Superiores8JMKD3MGPCW/3EUUDJE
DivulgaçãoWEBSCI; PORTALCAPES; COMPENDEX; SCOPUS.
Acervo Hospedeirosid.inpe.br/mtc-m21b/2013/09.26.14.25.20
Área de notas
Campos Vaziosalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel electronicmailaddress format isbn lineage mark nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress project resumeid rightsholder secondarydate secondarykey session shorttitle sponsor subject targetfile tertiarymark tertiarytype typeofwork url
Área de identificação
Tipo de ReferênciaJournal Article
Sitemtc-m16d.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP7W/3E9B97F
Repositóriosid.inpe.br/mtc-m19/2013/06.09.02.30.58
Última Atualização2013:07.16.17.46.51 administrator
Metadadossid.inpe.br/mtc-m19/2013/06.09.02.30.59
Última Atualização dos Metadados2018:06.05.04.14.13 administrator
DOI10.1051/0004-6361/201220448
ISSN0004-6361
1432-0746
Rótuloscopus
Chave de CitaçãoCarrubaHuamDomiRoig:2013:IIRe10
TítuloChaotic diffusion caused by close encounters with several massive asteroids: II. the regions of (10) Hygiea, (2) Pallas, and (31) Euphrosyne
ProjetoCNPq (305453/2011-4); FAPESP (11/19863-3); CAPES (23038.007093/2012-13).
Ano2013
MêsFeb.
Data de Acesso24 fev. 2021
Tipo de Trabalhojournal article
Número de Arquivos1
Tamanho1103 KiB
Área de contextualização
Autor1 Carruba, V.
2 Huaman, M.
3 Domingos, Rita de Cássia
4 Roig, F.
Grupo1
2
3 ETE-ETE-INPE-MCTI-GOV-BR
Afiliação1 UNESP, Univ. Estadual Paulista, Grupo de Dinâmica Orbital e Planetologia, Guaratinguetá, SP, 12516-410, Brazil
2 UNESP, Univ. Estadual Paulista, Grupo de Dinâmica Orbital e Planetologia, Guaratinguetá, SP, 12516-410, Brazil
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 ON, Observatório Nacional, Rio de Janeiro, RJ, 20921-400, Brazil
Endereço de e-Mailmarcelo.pazos@inpe.br
RevistaAstronomy & Astrophysics
Volume550
NúmeroA85
Páginas1-10
Tipo SecundárioPRE PI
Histórico2018-06-05 04:14:13 :: administrator -> marcelo.pazos@inpe.br :: 2013
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãopublisher
Palavras-Chavecelestial mechanics, chaotic diffusion, drift rates, high rate, minor bodies, minor planets, asteroids, minor planets, non-gravitational force, orbital evolutions, relative velocity, scattering effects, semimajor axis, significant mechanism, symplectic integrators, asteroids.
ResumoContext. Close encounters with (1) Ceres and (4) Vesta, the two most massive bodies in the main belt, are known to be a mechanism of dynamical mobility able to significantly alter proper elements of minor bodies, and they are the main source of dynamical mobility for medium-sized and large asteroids (D > 20 km, approximately). Recently, it has been shown that drift rates caused by close encounters with massive asteroids may change significantly on timescales of 30 Myr when different models (i.e., different numbers of massive asteroids) are considered. Aims. So far, not much attention has been given to the case of diffusion caused by the other most massive bodies in the main belt: (2) Pallas, (10) Hygiea, and (31) Euphrosyne, the third, fourth, and one of the most massive highly inclined asteroids in the main belt, respectively. Since (2) Pallas is a highly inclined object, relative velocities at encounter with other asteroids tend to be high and changes in proper elements are therefore relatively small. It was thus believed that the scattering effect caused by highly inclined objects in general should be small. Can diffusion by close encounters with these asteroids be a significant mechanism of long-term dynamical mobility? Methods. By performing simulations with symplectic integrators, we studied the problem of scattering caused by close encounters with (2) Pallas, (10) Hygiea, and (31) Euphrosyne when only the massive asteroids (and the eight planets) are considered, and the other massive main belt asteroids and non-gravitational forces are also accounted for. Results. By finding relatively small values of drift rates for (2) Pallas, we confirm that orbital scattering by this highly inclined object is indeed a minor effect. Unexpectedly, however, we obtained values of drift rates for changes in proper semi-major axis a caused by (10) Hygiea and (31) Euphrosyne larger than what was previously found for scattering by (4) Vesta. These high rates may have repercussions on the orbital evolution and age estimate of their respective families. © 2013 ESO.
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ArranjoBDMCI > Fonds > Produção > CGETE > Chaotic diffusion caused...
Conteúdo da Pasta sourcenão têm arquivos
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URL dos dadoshttp://urlib.net/rep/8JMKD3MGP7W/3E9B97F
URL dos dados zipadoshttp://urlib.net/zip/8JMKD3MGP7W/3E9B97F
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Arquivo Alvoaa20448-12_tap.pdf
Grupo de Usuáriosadministrator
marcelo.pazos@inpe.br
Grupo de Leitoresadministrator
marcelo.pazos@inpe.br
Visibilidadeshown
Política de Arquivamentoallowpublisher allowfinaldraft
Permissão de Leituraallow from all
Permissão de Atualizaçãonão transferida
Área de fontes relacionadas
Repositório Espelhoiconet.com.br/banon/2006/11.26.21.31
Unidades Imediatamente Superiores8JMKD3MGPCW/3EUUDJE
DivulgaçãoWEBSCI; PORTALCAPES; MGA; COMPENDEX; SCOPUS.
Acervo Hospedeirosid.inpe.br/mtc-m19@80/2009/08.21.17.02
Área de notas
Campos Vaziosalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel electronicmailaddress format isbn lineage mark nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress resumeid rightsholder secondarydate secondarykey secondarymark session shorttitle sponsor subject tertiarymark tertiarytype url
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