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dc.contributor.authorSing, David K.
dc.contributor.authorGreen, E.M.
dc.contributor.authorHowell, S.B.
dc.contributor.authorHolberg, J.B.
dc.contributor.authorLopez-Morales, M.
dc.contributor.authorShaw, J.S.
dc.contributor.authorSchmidt, G.D.
dc.date.accessioned2014-12-17T09:59:42Z
dc.date.issued2007
dc.description.abstractAims.We report on the discovery of J0644+3344 , a bright, deeply-eclipsing cataclysmic variable (CV) binary. Methods.Optical photometric and spectroscopic observations were obtained to determine the nature and characteristics of this CV. Results. Spectral signatures of both binary components and an accretion disk can be seen at optical wavelengths. The optical spectrum shows broad H I, He I, and He II accretion disk emission lines with deep narrow absorption components from H I, He I, Mg II, and Ca II. The absorption lines are seen throughout the orbital period, disappearing only during primary eclipse. These absorption lines are either the result of an optically-thick inner accretion disk or from the photosphere of the primary star. Radial velocity measurements show that the H I, He I, and Mg II absorption lines phase with the primary star, while weak absorption features in the continuum, between Hα and Hβ, phase with the secondary star. Radial velocity solutions give a 150 ± km s1 semi-amplitude for the primary star and 192.8 ± 5.6 km s-1 for the secondary, resulting in a primary to secondary mass ratio of q = 1.285. The individual stellar masses are 0.63-0.69 M⊙ for the primary and 0.49-0.54 M⊙ for the secondary, with the uncertainty largely due to the inclination. Conclusions. The bright eclipsing nature of this binary has helped provide masses for both components with an accuracy rarely achieved for CVs. This binary most closely resembles a nova-like UX UMa or SW Sex type of CV. J0644+3344 , however, has a longer orbital period than most UX UMa or SW Sex stars. Assuming an evolution toward shorter orbital periods, J0644+3344 is therefore likely to be a young interacting binary. The secondary star is consistent with the size and spectral type of a K8 star, but has the mass of a M0.en_GB
dc.description.sponsorshipCNESen_GB
dc.identifier.citationVol. 474 (3), pp. 951-960en_GB
dc.identifier.doi10.1051/0004-6361:20078026
dc.identifier.urihttp://hdl.handle.net/10871/16068
dc.language.isoenen_GB
dc.publisherEDP Sciences for European Southern Observatory (ESO)en_GB
dc.relation.urlhttp://dx.doi.org/10.1051/0004-6361:20078026en_GB
dc.subjectaccretion, accretion disksen_GB
dc.subjectstars: binaries: eclipsingen_GB
dc.subjectstars: novae, cataclysmic variablesen_GB
dc.titleDiscovery of a bright eclipsing cataclysmic variableen_GB
dc.typeArticleen_GB
dc.date.available2014-12-17T09:59:42Z
dc.identifier.issn0004-6361
dc.descriptionCopyright © ESO 2007en_GB
dc.identifier.eissn1432-0746
dc.identifier.journalAstronomy and Astrophysicsen_GB


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