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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/65661
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dc.creatorMateus de Souza Angelopt_BR
dc.creatorJoão Francisco Coelho dos Santos Juniorpt_BR
dc.creatorFrancisco Ferreira de Souza Maiapt_BR
dc.creatorWagner José Corradi Barbosapt_BR
dc.date.accessioned2024-03-11T17:15:54Z-
dc.date.available2024-03-11T17:15:54Z-
dc.date.issued2022-
dc.citation.volume510pt_BR
dc.citation.issue4pt_BR
dc.citation.spage5695pt_BR
dc.citation.epage5724pt_BR
dc.identifier.doihttps://doi.org/10.1093/mnras/stab3807pt_BR
dc.identifier.issn1365-2966pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/65661-
dc.description.resumoA number of stellar open cluster (OC) pairs in the Milky Way occupy similar positions in the phase space (coordinates, parallax, and proper motions) and therefore may constitute physically interacting systems. The characterization of such objects based on observational data is a fundamental step towards a proper understanding of their physical status and to investigate cluster pair formation in the Galaxy. In this work, we employed the Gaia EDR3 data to investigate a set of 16 OCs distributed as 7 stellar aggregates. We determined structural parameters and applied a decontamination technique that allowed us to obtain unambiguous lists of member stars. The studied OCs span Galactocentric distances and ages in the ranges of and ⁠. Eight OCs were found to constitute four gravitationally bound pairs (NGC 5617–Trumpler 22, Collinder 394–NGC 6716, Ruprecht 100–Ruprecht 101, and NGC 659–NGC 663, the latter being a dynamically unevolved binary) and other four clusters constitute two interacting, but gravitationally unbound, pairs (King 16–Berkeley 4 and NGC 2383–NGC 2384, the latter being a dissolving OC). Other four OCs (Dias 1, Pismis 19, Czernik 20, and NGC 1857) seem not associated with any stellar aggregates. Apparently, clusters within bound and dynamically evolved pairs tend to present ratios of half-light to tidal radius larger than single clusters located at similar RG, suggesting that mutual tidal interactions may possibly affect their structural parameters. Unbound or dynamically unevolved systems seem to present less noticeable signature of tidal forces on their structure. Moreover, the core radius seems more importantly correlated with the clusters’ internal dynamical relaxation process.pt_BR
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológicopt_BR
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Geraispt_BR
dc.description.sponsorshipCAPES - Coordenação de Aperfeiçoamento de Pessoal de Nível Superiorpt_BR
dc.format.mimetypepdfpt_BR
dc.languageengpt_BR
dc.publisherUniversidade Federal de Minas Geraispt_BR
dc.publisher.countryBrasilpt_BR
dc.publisher.departmentICX - DEPARTAMENTO DE FÍSICApt_BR
dc.publisher.initialsUFMGpt_BR
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.rightsAcesso Abertopt_BR
dc.subjectGaiapt_BR
dc.subjectOpen clusters and associationspt_BR
dc.subjectGalaxypt_BR
dc.subject.otherAglomerado de estrelaspt_BR
dc.titleInvestigating galactic binary cluster candidates with Gaia EDR3pt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://academic.oup.com/mnras/article/510/4/5695/6496042pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-6138-0674pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-1794-6356pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-2569-4032pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5150-5282pt_BR
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