Elemental abundances of the supergiant stars sigma Cygnus and eta Leonis

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dc.contributor.authorTanriverdi, Taner
dc.date.accessioned2019-08-01T13:38:39Z
dc.date.available2019-08-01T13:38:39Z
dc.date.issued2013
dc.departmentNiğde ÖHÜ
dc.description.abstractThis study aims to analyse the elemental abundances for the late B type supergiant star sigma Cyg and the early A-type supergiant eta Leo using ATLAS9 (Kurucz, 1995; Sbordone et al., 2004), assuming local thermodynamic equilibrium (LTE). The spectra used in this study are obtained from Dominion Astrophysical Observatory and have high resolution and signal-to-noise ratios. The effective temperature and the surface gravity of a Cyg are determined from the ionisation equilibria of Al I/II Mg I/II, Fe I/II, Fe and by fitting to the wings of Hy and Hp profiles as T-eff = 10388 K and log g = 1.80. The elemental abundances of eta Leo are determined using T-eff = 9600 K and log g = 2.00, as reported by Przybilla et al. (2006). The ionisation equilibria of C I/II, N I/II, Mg I/II, Ca I/II, Cr I/II and Fe I/II/III are also satisfied in the atmosphere of eta Leo. The radial velocities of sigma Cyg and eta Leo are -7.25 +/- 7.57 km s(-1) and 10.40 +/- 13.37 km s(-1), respectively, The derived projected rotational velocities vsini from synthetic spectra are 27 and 2 km s(-1) for both stars, respectively. The macroturbulent velocities (zeta) are 24 2 km s(-1) and 14.5 +/- 1.5 km s(-1). Also, the microturbulent velocities (xi) have been determined for both of stars as 3.5 km s(-1). The CNO abundance results of sigma Cyg and eta Leo show C deficiency, N overabundance and O in excess. (C) 2013 Elsevier B.V. All rights reserved.
dc.description.sponsorshipAnkara University
dc.description.sponsorshipI am thankful to James E. Hesser and the directory of the DAD (Dominion Astrophysical Observatory) for the observing time. This research utilised the SIMBAD database, which is operated at CDS, Strasbourg, France. I am also indebted to Dr. Saul J. Adelman for contributing the spectra from DAD to help this study. I am grateful to Dr. B. Albayrak for his help during this study. Ankara University is also gratefully acknowledged for the support given to this research. A special thanks to the anonymous referees of this paper for careful reading of the manuscript and their generous comments.
dc.identifier.doi10.1016/j.newast.2013.03.013
dc.identifier.endpage67
dc.identifier.issn1384-1076
dc.identifier.issn1384-1092
dc.identifier.scopus2-s2.0-84877776097
dc.identifier.scopusqualityQ3
dc.identifier.startpage50
dc.identifier.urihttps://dx.doi.org/10.1016/j.newast.2013.03.013
dc.identifier.urihttps://hdl.handle.net/11480/4319
dc.identifier.volume25
dc.identifier.wosWOS:000322805300009
dc.identifier.wosqualityQ3
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.institutionauthorTanriverdi, Taner
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.subjectSupergiants-stars
dc.subjectIndividuals: (sigma Cyg, eta Leo) stars
dc.subjectAbundances-technique: spectroscopic
dc.titleElemental abundances of the supergiant stars sigma Cygnus and eta Leonis
dc.typeArticle

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