Active binary R Arae revisited: Bringing the secondary component to light and physical modelling of the circumstellar material

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dc.authoridBAKIS, VOLKAN/0000-0002-3125-9010
dc.contributor.authorBakis, H.
dc.contributor.authorBakis, V.
dc.contributor.authorEker, Z.
dc.contributor.authorDemircan, O.
dc.date.accessioned2025-01-27T21:03:54Z
dc.date.available2025-01-27T21:03:54Z
dc.date.issued2016
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThe spectral lines of the secondary component of the active binary system R Ara were uncovered for the first time, which allowed directly to determine the parameters of the spectroscopic orbit. The mass ratio of the system is updated to a new observational value of M-2/M-1 = 0.305 +/- 0.005 which is similar to 20 per cent smaller than the literature value (M-2/M-1 = 0.39). Modelling the reconstructed component spectra yielded the equatorial rotational velocities of the components as nu(rot1) = 202 km s(-1) and nu(rot2) = 73 km s(-1) indicating a very fast rotation (similar to 5 times faster than the synchronous rotation velocity) for the primary and synchronous rotation for the secondary component. The circumstellar material in the system was investigated using the Hipparcossatellite data and the high-resolution (R similar to 41 000) spectral data. According to our model, there is always material transferring from the secondary component on to the primary causing a hot region on its surface. The structural difference between the spectra taken at the same orbital phase but at different epochs proved that the density and the velocity of the transferring material are variable. There are three main trends in the light curve and spectral line variations suggesting the activity cycles for the system, namely quiescent, moderate and, active cycles. It was estimated that the circumstellar material around could be extended to large distances up to 40 R-circle dot from the system.
dc.identifier.doi10.1093/mnras/stw320
dc.identifier.endpage516
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue1
dc.identifier.scopus2-s2.0-84963774320
dc.identifier.scopusqualityQ1
dc.identifier.startpage508
dc.identifier.urihttps://doi.org/10.1093/mnras/stw320
dc.identifier.urihttps://hdl.handle.net/20.500.12428/27490
dc.identifier.volume458
dc.identifier.wosWOS:000374568900033
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.subjectaccretion
dc.subjectaccretion discs
dc.subjectbinaries: eclipsing
dc.subjectcircumstellar matter
dc.subjectstars: individual: (R Ara)
dc.titleActive binary R Arae revisited: Bringing the secondary component to light and physical modelling of the circumstellar material
dc.typeArticle

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