NGC 6124: a young open cluster with anomalous-and fast-rotating giant stars

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dc.creatorNacizo Holanda
dc.creatorNatalia Drake
dc.creatorWagner José Corradi Barbosa
dc.creatorF. A. Ferreira
dc.creatorFrancisco Maia
dc.creatorLaura Magrini
dc.creatorJ. R. P. da Silva
dc.creatorC. B. Pereira
dc.date.accessioned2023-04-12T20:54:23Z
dc.date.accessioned2025-09-09T00:58:50Z
dc.date.available2023-04-12T20:54:23Z
dc.date.issued2021
dc.identifier.doihttps://doi.org/10.1093/mnras/stab2836
dc.identifier.issn00358711
dc.identifier.urihttps://hdl.handle.net/1843/51883
dc.languagepor
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsAcesso Restrito
dc.subjectEstrelas
dc.subjectGalaxias - Aglomerados
dc.subject.otherStars:abundances
dc.subject.otherOtars:fundamentalparameters
dc.subject.otherGalaxy:disc
dc.subject.otherOpen clusters
dc.subject.otherAssociations: individual: NGC 6124
dc.titleNGC 6124: a young open cluster with anomalous-and fast-rotating giant stars
dc.typeArtigo de periódico
local.citation.epage5801
local.citation.issue4
local.citation.spage5786
local.citation.volume508
local.description.resumoWe present the results of a chemical analysis of fast and anomalous rotator giants members of the young open cluster NGC6124. For this purpose, we carried out abundances of the mixing sensitive species such as Li, C, N, Na, and 12C/13C isotopic ratio, as well as other chemical species for a sample of four giants among the seven observed ones. This study is based on standard spectral analysis technique using high-resolution spectroscopic data. We also performed an investigation of the rotational velocity (v sin i) once this sample exhibits abnormal values–giant stars commonly present rotational velocities of few kms−1. In parallel, we have performed a membership study, making use of the third data release from ESA Gaia mission. Based on these data, we estimated a distance of d = 630pc and an age of 178Myr through isochrone fitting. After that procedure, we matched all the information raised and investigated the evolutionary stages and thermohaline mixing model through of spectroscopic Teff and log g and mixing tracers, such as 12C/13C and Na, of the studied stars. We derived a low mean metallicity of [Fe/H] = −0.13 ± 0.05 and a modest enhancement of the elements created by the s-process, such as Y, Zr, La, Ce, and Nd, which is in agreement with what has already been reported in the literature for young clusters. The giants analysed have homogeneous abundances, except for lithium abundance [log (Li)NLTE = 1.08 ± 0.42] and this may be associated with a combination of mechanisms that act increasing or decreasing lithium abundances in stellar atmospheres.
local.identifier.orcidhttps://orcid.org/0000-0002-8504-6248
local.identifier.orcidhttps://orcid.org/0000-0003-4842-8834
local.identifier.orcidhttps://orcid.org/0000-0002-5150-5282
local.identifier.orcidhttps://orcid.org/0000-0002-4998-4624
local.identifier.orcidhttps://orcid.org/0000-0003-4486-6802
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://academic.oup.com/mnras/article/508/4/5786/6381707

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