BSN. V. The First Detailed Light Curve Modeling of Eight Totally Eclipsing Contact Binary Stars Using Ground-based and TESS Observations

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dc.authorid0000-0002-7348-8815
dc.authorid0000-0002-0196-9732
dc.contributor.authorPoro, Atila
dc.contributor.authorMichel, Raul
dc.contributor.authorJavier Tamayo, Francisco
dc.contributor.authorHedayatjoo, Mahya
dc.contributor.authorAceves, Hector
dc.contributor.authorAlicavus, Fahri
dc.date.accessioned2026-02-03T12:02:21Z
dc.date.available2026-02-03T12:02:21Z
dc.date.issued2025
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThis study broadens our comprehensive investigation of total-eclipse W Ursae Majoris-type contact binaries by analyzing eight additional systems, continuing our previous research. Multiband BV RcIc photometric data were obtained at an observatory in Mexico, from which new times of minima were determined. All target systems also had available space-based Transiting Exoplanet Survey Satellite time-series data. Orbital period variations were studied for eight target systems, showing either linear or parabolic trends. The target systems exhibiting parabolic trends demonstrated a sustained decrease in their orbital periods over time. We modeled the light curves utilizing the PHOEBE Python code in combination with the BSN application. We revisited the relationship between orbital period and the temperature of the hotter component in contact binary systems using an empirical approach. Our analysis identified a clear break at P = 0.27 day, separating the systems into two distinct groups for orbital periods shorter than 0.6 day. Following the determination of stellar extinction, absolute parameters for seven systems were estimated employing parallax measurements from Gaia DR3. Based on the components' effective temperatures and masses, the systems were classified into A- and W-subtypes. Their evolutionary states were illustrated using mass-radius and mass-luminosity diagrams.
dc.identifier.doi10.1088/1538-3873/ae288b
dc.identifier.issn0004-6280
dc.identifier.issn1538-3873
dc.identifier.issue12
dc.identifier.urihttps://doi.org/10.1088/1538-3873/ae288b
dc.identifier.urihttps://hdl.handle.net/20.500.12428/34713
dc.identifier.volume137
dc.identifier.wosWOS:001642616000001
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.language.isoen
dc.publisherIop Publishing Ltd
dc.relation.ispartofPublications of the Astronomical Society of the Pacific
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanı
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WOS_20260130
dc.subjectVariable-Stars
dc.subjectOrbital Period
dc.subjectMass
dc.subjectEvolution
dc.subjectSystems
dc.subjectExplanation
dc.subjectNorthern
dc.subjectCatalog
dc.subjectPhysics
dc.subjectLimit
dc.titleBSN. V. The First Detailed Light Curve Modeling of Eight Totally Eclipsing Contact Binary Stars Using Ground-based and TESS Observations
dc.typeArticle

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