Nature of the oscillating semi-detached eclipsing binary system IO Ursae Majoris

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dc.authoridSoydugan, Faruk/0000-0002-5141-7645
dc.authoridLiakos, Alexios/0000-0002-0490-1469
dc.contributor.authorSoydugan, Faruk
dc.contributor.authorSoydugan, Esin
dc.contributor.authorKanvermez, C.
dc.contributor.authorLiakos, A.
dc.date.accessioned2025-01-27T20:12:27Z
dc.date.available2025-01-27T20:12:27Z
dc.date.issued2013
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThis paper presents results from analysing spectroscopic and multicolour photometric observations of the neglected semi-detached eclipsing binary system IO Ursae Majoris (IO UMa). For the first time, the orbital parameters of the system and fundamental physical properties of its components were determined from simultaneous analysis of BVR light curves and radial velocities of the components. The masses and radii of the primary and secondary components were found to be M-1 = 2.11 +/- 0.07 M-circle dot, M-2 = 0.29 +/- 0.02 M-circle dot and R-1 = 3.00 +/- 0.04 R-circle dot and R-2 = 3.92 +/- 0.05 R-circle dot, respectively. Derived absolute parameters yield the photometric distance of IO UMa as 263 +/- 13 pc. The projected rotational velocity of the mass-accreting hotter component was measured as 34.5 +/- 2 km s(-1), just 1.28 times faster than the synchronous value. The hotter component of the system, located in the region of the instability strip, indicates pulsational variation with short period and small amplitude. Frequency analysis after subtracting the theoretical light curve from photometric data revealed that the more massive component shows delta Scuti type pulsation with four detected frequencies. The total amplitude of the variation in the V filter was found to be 0.03 mag. Mode identification using amplitude ratios and phase differences in different filters suggests that the main pulsation frequency of 22.0148 d(-1) is probably a radial mode.
dc.description.sponsorshipScientific and Technological Research Council of Turkey (TUBITAK) [111T224, 107T634]; Canakkale Onsekiz Mart University Science Foundation [2011/014]
dc.description.sponsorshipThe authors would like to thank the staff of the Catania Astrophysical Observatory for their kind hospitality, the allocation of telescope time and assistance during observations. We wish to thank the referee for the substantial suggestions and comments that enabled us to improve the manuscript considerably. We also thank the Scientific and Technological Research Council of Turkey (TUBITAK, Grant Nos 111T224 and 107T634) and Canakkale Onsekiz Mart University Science Foundation (Project No. 2011/014) for supporting this study. The current research is part of the MSc thesis of CK. This research made use of the VIZIER and SIMBAD data bases at CDS, Strasbourg, France.
dc.identifier.doi10.1093/mnras/stt678
dc.identifier.endpage3287
dc.identifier.issn0035-8711
dc.identifier.issue4
dc.identifier.scopus2-s2.0-84880018496
dc.identifier.scopusqualityQ1
dc.identifier.startpage3278
dc.identifier.urihttps://doi.org/10.1093/mnras/stt678
dc.identifier.urihttps://hdl.handle.net/20.500.12428/20948
dc.identifier.volume432
dc.identifier.wosWOS:000321053500055
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.subjectbinaries: eclipsing
dc.subjectstars: fundamental parameters
dc.subjectstars: individual: IO UMa
dc.titleNature of the oscillating semi-detached eclipsing binary system IO Ursae Majoris
dc.typeArticle

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