Modelling of eclipsing binary systems with pulsating components and tertiary companions: BF Vel and RR Lep

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dc.contributor.authorLiakos, A.
dc.contributor.authorMoriarty, D. J. W.
dc.contributor.authorErdem, A.
dc.contributor.authorWest, J. F.
dc.contributor.authorEvans, P.
dc.date.accessioned2025-01-27T20:24:36Z
dc.date.available2025-01-27T20:24:36Z
dc.date.issued2024
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThis research paper presents a comprehensive analysis of RR Lep and BF Vel, two southern short-period, semi-detached, oscillating Algols (oEA stars) that have been shown to be triple systems. We determined the spectral types of the primary components and calculated the radial velocities from spectra observed with the Australian National University's 2.3 m telescope and Wide Field Spectrograph. The spectra of the Na I D doublet confirmed the presence of tertiary components that were apparent in the broadening function analyses. During primary eclipses chromospherical activity in their secondary components was apparent in their H-alpha spectra; it was also apparent in the Na I D spectra of BF Vel with its almost complete annular eclipse. Ground-based telescopes were used for observations in several pass bands for photometric analyses. These observations were complemented by data from the Transiting Exoplanet Survey Satellite (TESS) mission, allowing us to model the light curves, followed by a detailed analysis of pulsations. Eclipse-timing variation (ETV) analyses of both systems were used to determine the most likely mechanisms modulating the orbital period. We found mass values of M-1 = 2.9 M-circle dot and M-2 = 0.75 M-circle dot for the components of RR Lep, along with M-1 = 1.93 M-circle dot and M-2 = 0.97 M-circle dot for those of BF Vel. By integrating information from photometry, spectroscopy, and ETV analysis, we found that tertiary components revolve around both systems. The primary star of RR Lep pulsates in 36 frequencies; of these, five were identified as independent modes, with the dominant one being 32.28 d(-1). The pulsating component of BF Vel oscillates in 37 frequencies, with the frequency 46.73 d(-1) revealed as the only independent mode. For both systems, a number of frequencies were found to be related to the orbital frequency. Their physical properties were compared with other oEA stars in mass-radius and Hertzsprung-Russell diagrams, while the pulsational properties of their delta Sct components were compared with currently known systems of this type within the orbital-pulsation period and logg-pulsation period diagrams.
dc.description.sponsorshipAstronomical Association of Queensland; NASA Explorer Program [5094]; NOA's internal fellowship 'SPECIES'; Edward Corbould Research Fund of the Astronomical Association of Queensland
dc.description.sponsorshipIt is a pleasure to express our appreciation of the high quality and ready availability, via the Mikulski Archive for Space Telescopes (MAST), of data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. This research partly made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. A. L. acknowledges financial support from the NOA's internal fellowship 'SPECIES' (No. 5094). D. J. W. M. and J. F. W. acknowledge grants for time on the ANU 2.3 m telescope from the Edward Corbould Research Fund of the Astronomical Association of Queensland. D. J. W. M. is grateful to Prof. Michael Drinkwater for his extensive assistance with the planning and data analysis of the ANU 2.3 m telescope observations. D. J. W. M. thanks C. M. Moriarty, A. Mohit, Y. Rist, L. Coetzee, and S. Sweet for their assistance with the spectroscopic observations. We thank the anonymous reviewer for the valuable comments that improved the quality of this work.
dc.identifier.doi10.1051/0004-6361/202450560
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.scopus2-s2.0-85210290160
dc.identifier.scopusqualityQ1
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202450560
dc.identifier.urihttps://hdl.handle.net/20.500.12428/22290
dc.identifier.volume691
dc.identifier.wosWOS:001360344100014
dc.identifier.wosqualityN/A
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherEdp Sciences S A
dc.relation.ispartofAstronomy & Astrophysics
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectbinaries: close
dc.subjectbinaries: eclipsing
dc.subjectstars: fundamental parameters
dc.subjectstars: individual: BF Vel
dc.subjectstars: individual: RR Lep
dc.subjectstars: variables: delta Scuti
dc.titleModelling of eclipsing binary systems with pulsating components and tertiary companions: BF Vel and RR Lep
dc.typeArticle

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