On the nature of the eccentric eclipsing binary star SY Phe with a pulsating ? Dor component

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dc.authoridERDEM, Ahmet/0000-0001-5289-8850
dc.contributor.authorErdem, Ahmet
dc.contributor.authorSurgit, Derya
dc.contributor.authorEngelbrecht, Chris A.
dc.contributor.authorZasche, Petr
dc.contributor.authorBakis, Volkan
dc.contributor.authorMarang, Fred
dc.date.accessioned2025-01-27T20:44:03Z
dc.date.available2025-01-27T20:44:03Z
dc.date.issued2024
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractSpectroscopic observations of the eccentric binary system SY Phe were made at the South African Astronomical Observatory in 2019, 2020, and 2021, and its mid-resolution spectra were obtained. The radial velocities of the component stars were measured using the cross-correlation method and Fourier disentangling of the spectra. The spectral type (hence the effective temperature) of the primary star was determined from a model-atmosphere analysis. The radial velocity and Transiting Exoplanet Survey Satellite ( TESS ) light curves of the system were analysed, and its absolute parameters were derived. A strong (5.2 mmag) periodic signal with a frequency typical of gamma Dor stars (1.169 cycles per day) dominates the Fourier spectrum of the light curve between the eclipses. Apsidal motion parameters of SY Phe were calculated by studying eclipse timing variations. The Geneva evolution models indicate an evolutionary age of 2 Gyr and solar metallicity for the primary component; however, although the position of the secondary component in the H-R diagram matches the isochrone of 2Gyr, it appears to have a larger radius and higher effective temperature than expected for its determined mass. Here, the secondary component has too large a radius, which is in accordance with the radius discrepancy problem that has been encountered in other studies, especially in late-type dwarfs, and has not been solved for half a century.
dc.description.sponsorshipTUEBITAK (Scientific and Technological Research Council of Tuerkiye) [121F203]; South African National Research Foundation; University of Johannesburg
dc.description.sponsorshipThis research was supported by TUEBITAK (Scientific and Technological Research Council of Tuerkiye) under grant no. 121F203. CAE thanks the South African National Research Foundation and the University of Johannesburg for financial support. All the authors thank the SAAO for observing time. We also thank the unnamed referee for informative and helpful comments.
dc.identifier.doi10.1093/mnras/stae2374
dc.identifier.endpage418
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue1
dc.identifier.scopus2-s2.0-85208126073
dc.identifier.scopusqualityQ1
dc.identifier.startpage406
dc.identifier.urihttps://doi.org/10.1093/mnras/stae2374
dc.identifier.urihttps://hdl.handle.net/20.500.12428/24464
dc.identifier.volume535
dc.identifier.wosWOS:001345568500011
dc.identifier.wosqualityN/A
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.subjectbinaries: eclipsing
dc.subjectstars: fundamental parameters
dc.subjectstars: individual: SY Phe
dc.subjectstars: oscillations
dc.subjectstars: variables: Gamma Doradus
dc.titleOn the nature of the eccentric eclipsing binary star SY Phe with a pulsating ? Dor component
dc.typeArticle

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