High-resolution spectroscopy and abundance analysis of ? Scuti stars near the ? Doradus instability strip

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dc.authoridKahraman Alicavus, Filiz/0000-0002-9036-7476
dc.contributor.authorKahraman Alicavus, F.
dc.contributor.authorNiemczura, E.
dc.contributor.authorPolinska, M.
dc.contributor.authorHelminiak, K. G.
dc.contributor.authorLampens, P.
dc.contributor.authorMolenda-Zakowicz, J.
dc.contributor.authorUkita, N.
dc.date.accessioned2025-01-27T20:14:43Z
dc.date.available2025-01-27T20:14:43Z
dc.date.issued2017
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractdelta Scuti stars are remarkable objects for asteroseismology. In spite of decades of investigations, there are still important questions about these pulsating stars to be answered, such as their positions in log T-eff-log g diagram, or the dependence of the pulsation modes on atmospheric parameters and rotation. Therefore, we performed a detailed spectroscopic study of 41 delta Scuti stars. The selected objects are located near the gamma Doradus instability strip to make a reliable comparison between both types of variables. Spectral classification, stellar atmospheric parameters T-eff, log g, xi) and v sin i values were determined. The spectral types and luminosity classes of stars were found to be A1-F5 and III-V, respectively. The T-eff ranges from 6600 to 9400 K, whereas the obtained log g values are from 3.4 to 4.3. The v sin i values were found between 10 and 222 km s(-1). The derived chemical abundances of delta Scuti stars were compared to those of the non-pulsating stars and gamma Doradus variables. It turned out that both delta Scuti and gamma Doradus variables have similar abundance patterns, which are slightly different from the non-pulsating stars. These chemical differences can help us to understand why there are non-pulsating stars in classical instability strip. Effects of the obtained parameters on pulsation period and amplitude were examined. It appears that the pulsation period decreases with increasing T-eff. No significant correlations were found between pulsation period, amplitude and v sin i.
dc.description.sponsorshipScientific and Technological Research Council of Turkey (TUBITAK) [2214-A, 2211-C]; NCN [2014/13/B/ST9/00902]; Wroclaw Centre for Networking and Supercomputing [214]; national institutions
dc.description.sponsorshipWe would like to thank the reviewer for useful comments and suggestions that helped to improve the publication. This work has been partly supported by the Scientific and Technological Research Council of Turkey (TUBITAK) grant numbers 2214-A and 2211-C. EN, MP, JMZ and KH acknowledge support from the NCN grant no. 2014/13/B/ST9/00902. The calculations have been carried out in Wroclaw Centre for Networking and Supercomputing (http://www.wcss.pl), grant no. 214. We are grateful to Dr D. Shulyak for putting the code for calculating SEDs at our disposal. We thank to Dr G. Catanzaro for putting the code for Balmer lines analysis at our disposal. This research has made use of the SIMBAD data base, operated at CDS, Strasbourq, France. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
dc.identifier.doi10.1093/mnras/stx1498
dc.identifier.endpage4420
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue4
dc.identifier.scopus2-s2.0-85046090492
dc.identifier.scopusqualityQ1
dc.identifier.startpage4408
dc.identifier.urihttps://doi.org/10.1093/mnras/stx1498
dc.identifier.urihttps://hdl.handle.net/20.500.12428/21183
dc.identifier.volume470
dc.identifier.wosWOS:000408207600046
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherOxford Univ Press
dc.relation.ispartofMonthly Notices of The Royal Astronomical Society
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectstars: abundances
dc.subjectstars: chemically peculiar
dc.subjectstars: general
dc.subjectstars: rotation
dc.subjectstars: variables: delta Scuti
dc.titleHigh-resolution spectroscopy and abundance analysis of ? Scuti stars near the ? Doradus instability strip
dc.typeArticle

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