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Chemical abundances in bright giants of the globular cluster M62 (NGC 6266)
dc.contributor.author | Yong, David | pt_BR |
dc.contributor.author | Alves-Brito, Alan | pt_BR |
dc.contributor.author | Da Costa, Gary Stewart | pt_BR |
dc.contributor.author | Alonso Garcia, Javier | pt_BR |
dc.contributor.author | Karakas, Amanda I. | pt_BR |
dc.contributor.author | Pignatari, Marco | pt_BR |
dc.contributor.author | Roederer, Ian U. | pt_BR |
dc.contributor.author | Aoki, Wako | pt_BR |
dc.contributor.author | Fishlock, Cherie K. | pt_BR |
dc.contributor.author | Grundahl, Frank | pt_BR |
dc.contributor.author | Norris, John E. | pt_BR |
dc.date.accessioned | 2014-09-19T02:14:30Z | pt_BR |
dc.date.issued | 2014 | pt_BR |
dc.identifier.issn | 0035-8711 | pt_BR |
dc.identifier.uri | http://hdl.handle.net/10183/103450 | pt_BR |
dc.description.abstract | With the exception of Terzan 5, all the Galactic globular clusters that possess significant metallicity spreads, such as ω Cen and M22, are preferentially the more luminous clusters with extended horizontal branches. Here we present radial velocities and chemical abundances for seven bright giants in the globular cluster M62, a previously little-studied cluster. With MV = −9.18, M62 is the ninth most luminous Galactic globular cluster and has an extended horizontal branch. Within our sample, we find (i) no evidence for a dispersion in metallicity, [Fe/H], beyond the measurement uncertainties, (ii) star-to-star abundance variations for C, O, Na and Al with the usual correlations between these elements as seen in other globular clusters, and (iii) a global enrichment for the elements Zr, Ba and La at the level [X/Fe] − ~ +0.4 dex. For elements heavier than La, the abundance ratios are consistent with the scaled-solar r-process distribution. Below La, the abundances are anomalous when compared to the scaled-solar s-process or r-process distributions. For these elements, the abundance signature in M62 is in agreement with predictions of the s-process from fast-rotating massive stars, although the high [Rb/Y] ratio we measure may be a challenge to this scenario. | en |
dc.format.mimetype | application/pdf | pt_BR |
dc.language.iso | eng | pt_BR |
dc.relation.ispartof | Monthly notices of the Royal Astronomical Society. Oxford. Vol. 439, no. 3 (Apr. 2014), p. 2638-2650 | pt_BR |
dc.rights | Open Access | en |
dc.subject | Stars: abundances | en |
dc.subject | Composicao estelar | pt_BR |
dc.subject | Estrelas gigantes | pt_BR |
dc.subject | Galaxy: abundances | en |
dc.subject | Aglomerados estelares globulares | pt_BR |
dc.subject | Globular clusters: individual: NGC 6266 | en |
dc.subject | Massa estelar | pt_BR |
dc.subject | Rotacao estelar | pt_BR |
dc.title | Chemical abundances in bright giants of the globular cluster M62 (NGC 6266) | pt_BR |
dc.type | Artigo de periódico | pt_BR |
dc.identifier.nrb | 000921576 | pt_BR |
dc.type.origin | Estrangeiro | pt_BR |
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