Characterizing the variability of a sample of massive stars in eclipsing binaries

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dc.authorid0000-0003-3119-0399
dc.authorid0000-0002-9036-7476
dc.authorid0000-0002-9382-2542
dc.authorid0000-0001-7756-1568
dc.authorid0000-0002-0004-0569
dc.contributor.authorEze, C. I.
dc.contributor.authorHandler, G.
dc.contributor.authorAlicavus, F. Kahraman
dc.contributor.authorPawar, T.
dc.contributor.authorMiszuda, A.
dc.date.accessioned2026-02-03T12:00:07Z
dc.date.available2026-02-03T12:00:07Z
dc.date.issued2025
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractMassive stars exhibit a perplexing mismatch between their inferred masses from different observational techniques, posing a significant challenge to our understanding of stellar evolution and structure. This discrepancy is believed to be caused by the underestimation of the convective core masses. The efficiency of such measurement is usually impaired by a lot of processes at work in the interior of the stars such as convective core overshooting and interior rotation. By integrating the precision of asteroseismology which provides insights into the internal structure and dynamics of stars, with the detailed observational constraints offered by eclipsing binary systems, this study aims to precisely characterize a sample of massive stars in eclipsing binaries to infer their properties and evolutionary state. In this paper, the sample, observed photometrically with TESS and spectroscopically with SALT HRS, CHIRON, HERMES and a spectrograph at Skalnate Pleso Observatory between 2021 and 2024, are analyzed. The orbital elements as well as the basic stellar parameters of the targets in the sample are fitted to derive the geometry of their orbits as well as their absolute parameters. The asteroseismic properties of the targets are also obtained, which unravel their core dynamics and profiles. This is a precursor work that provides detailed characterization of the targets in the sample for future theoretical modeling.
dc.description.sponsorshipPolish National Science Foundation (NCN) [2021/43/B/ST9/02972]
dc.description.sponsorshipAcknowledgements. The work is supported by the Polish National Science Foundation (NCN) under grant nr 2021/43/B/ST9/02972. C.I. Eze is grateful for the support received from the staff of the Stellar Department, Astronomical Institute of the Slovak Academy of Sciences during his observation runs at the Skalnate Pleso Observatory.
dc.identifier.doi10.31577/caosp.2025.55.3.452
dc.identifier.endpage461
dc.identifier.issn1335-1842
dc.identifier.issn1336-0337
dc.identifier.issue3
dc.identifier.scopus2-s2.0-105005872454
dc.identifier.scopusqualityQ4
dc.identifier.startpage452
dc.identifier.urihttps://doi.org/10.31577/caosp.2025.55.3.452
dc.identifier.urihttps://hdl.handle.net/20.500.12428/34520
dc.identifier.volume55
dc.identifier.wosWOS:001508471700005
dc.identifier.wosqualityQ4
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherSlovak Academy Sciences Astronomical Inst
dc.relation.ispartofContributions of the Astronomical Observatory Skalnate Pleso
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanı
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WOS_20260130
dc.subjectAsteroseismology
dc.subjectbinaries
dc.subjectmassive stars
dc.subjectstellar evolution
dc.subjectpulsations
dc.subjectrotation
dc.titleCharacterizing the variability of a sample of massive stars in eclipsing binaries
dc.typeArticle

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