New findings supporting the presence of a thick disc and bipolar jets in the ? Lyrae system

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dc.authoridSlechta, Miroslav/0000-0002-6819-2331
dc.authoridSkoda, Petr/0000-0002-7434-9518
dc.contributor.authorAk, H.
dc.contributor.authorChadima, P.
dc.contributor.authorHarmanec, P.
dc.contributor.authorDemircan, O.
dc.contributor.authorYang, S.
dc.contributor.authorKoubsky, P.
dc.contributor.authorSkoda, P.
dc.date.accessioned2025-01-27T20:59:52Z
dc.date.available2025-01-27T20:59:52Z
dc.date.issued2007
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractContext. Understanding large-scale mass exchange in binaries also requires studies of complicated objects in the rapid phases of the process. beta Lyr is one such object. Aims. Our goals were to analyse 52 photographic and 651 electronic spectra of beta Lyr to obtain additional information about circumstellar matter and to investigate spectrophotometric information for the first time. Methods. Improved quadratic ephemeris was derived via orbital solution with the FOTEL program. The spectra were disentangled using the KOREL program. Spectrophotometric quantities of 15 stronger absorption lines of the primary were measured and corrected for the orbital continuum variations using the fluxes calculated from a fit of the light curves with the BINSYN program. Central intensities of the V and R peaks of the Ha emission line were measured and corrected for the orbital light changes using the R-band light curve numerically modelled with the program PERIOD04. Results. Disentangling of photographic and electronic spectra led to the detection of weak absorption lines originating from the pseudophotosphere of the accretion disc. This way, a rich line spectrum of the accretion disc, not limited to only two previously known Si II 6347 and Si II 6371 lines, was obtained. A projected rotational velocity of 180 km s(-1) was estimated for the disc spectrum. Such a value agrees well with the assumption of the Keplerian rotation of the outer layers of the accretion disc. After the correction, a pronounced increase of the strength of all absorption lines around phases of the primary eclipse was found. We argue that this is due to additional absorption of the light of the primary in one of the jets and/or scattering envelope above the accretion disc of the gainer. The net intensity of the V peak of Ha shows no orbital variation, but a possible 271-d periodicity. The net intensity of the R peak shows mild orbital changes and a slow change over a cycle of about 2780 days. These results seem to support the earlier conclusion that the Ha emission originates in the jet-like structures. Conclusions. All new findings support the current picture that the circumstellar structures of beta Lyr consist of a thick accretion disc, bipolar jets, and a scattering envelope above the disc.
dc.identifier.doi10.1051/0004-6361:20065536
dc.identifier.endpage241
dc.identifier.issn1432-0746
dc.identifier.issue1
dc.identifier.scopus2-s2.0-33847008297
dc.identifier.scopusqualityQ1
dc.identifier.startpage233
dc.identifier.urihttps://doi.org/10.1051/0004-6361:20065536
dc.identifier.urihttps://hdl.handle.net/20.500.12428/26863
dc.identifier.volume463
dc.identifier.wosWOS:000243941900021
dc.identifier.wosqualityQ1
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.subjectstars : binaries : eclipsing
dc.subjectstars : individual : b Lyrae
dc.subjectbinaries : close
dc.subjectISM : jets and outflows
dc.titleNew findings supporting the presence of a thick disc and bipolar jets in the ? Lyrae system
dc.typeArticle

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