Abundance analysis of the supergiant stars HD 80057 and HD 80404 based on their UVES Spectra

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dc.authorid0000-0001-8600-4595
dc.contributor.authorTanriverdi, T.
dc.contributor.authorBasturk, O.
dc.date.accessioned2019-08-01T13:38:39Z
dc.date.available2019-08-01T13:38:39Z
dc.date.issued2016
dc.departmentNiğde ÖHÜ
dc.description.abstractThis study presents elemental abundances of the early A-type supergiant HD 80057 and the late A type supergiant HD 80404. High resolution and high signal-to-noise ratio spectra published by the UVES Paranal Observatory Project (Bagnulo et al., 2003)(1) were analyzed to compute their elemental abundances using ATLAS9 (Kurucz, 1993; 2005; Sbordone et al., 2004). In our analysis we assumed local thermodynamic equilibrium. The atmospheric parameters of HD 80057 used in this study are from Firnstein and Przybilla (2012), and that of HD 80404 are derived from spectral energy distribution, ionization equilibria of Cr and Fe I/II, the fits to the wings of Balmer and Paschen lines as T-eff = 7700 +/- 150 K and log g = 1.60 +/- 0.15 (in cgs). The microturbulent velocities of HD 80057 and HD 80404 have been determined as 4.3 +/- 0.1 and 2.2 +/- 0.0 km s(-1), respectively. The rotational velocities are 15 +/- 1 and 7 +/- 2 km s(-1) and their macroturbulence velocities are 24 +/- 2 and 2 +/- 1 km s(-1). We have given the abundances of 25 ions of 19 elements for HD 80057 and 36 ions of 25 elements for HD 80404. The abundances are close to solar values, except for some elements (Na, Sc, Ti, V, Ba, and Sr). We have found the metallicities [M/H] for HD 80057 and HD 80404 as -0.16 +/- 0.24 and -0.04 +/- 0.16 dex, respectively. The evolutionary status of these stars are discussed and their nitrogen-to-carbon (N/C) and nitrogen-to oxygen (N/O) ratios show that they are in their blue supergiant phase before the red supergiant region. (C) 2016 Elsevier B.V. All rights reserved.
dc.description.sponsorshipUVES Paranal Observatory Project (ESO DDT Program) [266.D-5655]
dc.description.sponsorshipThis research utilized the SIMBAD database, which is operated at CDS, Strasbourg, France. This work, made use of the MAST-IUE archive (http://archive.stsci.edu/iue/) of SAO/NASA ADS, is based on data obtained from UVES Paranal Observatory Project (ESO DDT Program ID 266.D-5655), of the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna. Atomic data compiled in the DREAM data base (E. Biemont, P. Palmeri & P. Quinet, Astrophys. Space Sci. 269-270, 635, 1999) were extracted via VALD (Kupka et al., 1999, and references therein). The authors thank the anonymous referee, whose useful comments helped to improve this work.
dc.identifier.doi10.1016/j.newast.2016.02.006
dc.identifier.endpage56
dc.identifier.issn1384-1076
dc.identifier.issn1384-1092
dc.identifier.scopus2-s2.0-84960194181
dc.identifier.scopusqualityQ3
dc.identifier.startpage46
dc.identifier.urihttps://dx.doi.org/10.1016/j.newast.2016.02.006
dc.identifier.urihttps://hdl.handle.net/11480/3599
dc.identifier.volume47
dc.identifier.wosWOS:000374426800009
dc.identifier.wosqualityQ3
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.institutionauthor[0-Belirlenecek]
dc.language.isoen
dc.publisherELSEVIER SCIENCE BV
dc.relation.ispartofNEW ASTRONOMY
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanı
dc.rightsinfo:eu-repo/semantics/closedAccess
dc.subjectStars: abundances
dc.subjectStars: individual: HD 80057
dc.subjectStars: individual: HD 80404
dc.subjectTechniques: spectroscopic
dc.titleAbundance analysis of the supergiant stars HD 80057 and HD 80404 based on their UVES Spectra
dc.typeArticle

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