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dc.contributor.authorCarter, P. J.
dc.contributor.authorSteeghs, D.
dc.contributor.authorMiguel Agustino, Enrique de 
dc.contributor.authorGoff, W.
dc.contributor.authorKoff, Robert
dc.contributor.authorKrajci, Thomas
dc.contributor.authorMarsh, T. R.
dc.contributor.authorGänsicke, B. T.
dc.contributor.authorBreedt, E.
dc.contributor.authorGroot, P. J.
dc.contributor.authorNelemans, G.
dc.contributor.authorRoelofs, G. H. A.
dc.contributor.authorRau, A.
dc.contributor.authorKoester, D.
dc.contributor.authorKupfer, T.
dc.identifier.citationCarter, P. J., Steeghs, D., Miguel Agustino, E., Goff, W., Koff, R., Krajci, T., Marsh, T. R., Gänsicke, B.,T., Breedt, E., Groot, P.,J., Nelemans, G., Roelofs, G.H.A., Rau, A., Koester, D., Kupfer, T.: "The helium-rich cataclysmic variable SBSS 1108+574". Vol. 431, n. 1, págs. 372-382, (2013). ISSN 0035-8711
dc.identifier.issn1365-2966 (electrónico)
dc.description.abstractWe present time-resolved spectroscopy and photometry of the dwarf nova SBSS 1108+574, obtained during the 2012 outburst. Its quiescent spectrum is unusually rich in helium, showing broad, double-peaked emission lines from the accretion disc. We measure a line flux ratio He i 5875/Hα = 0.81 ± 0.04, a much higher ratio than typically observed in cataclysmic variable stars (CVs). The outburst spectrum shows hydrogen and helium in absorption, with weak emission of Hα and He i 6678, as well as strong He ii emission. From our photometry, we find the superhump period to be 56.34 ± 0.18 min, in agreement with the previously published result. The spectroscopic period, derived from the radial velocities of the emission lines, is found to be 55.3 ± 0.8 min, consistent with a previously identified photometric orbital period, and significantly below the normal CV period minimum. This indicates that the donor in SBSS 1108+574 is highly evolved. The superhump excess derived from our photometry implies a mass ratio of q = 0.086 ± 0.014. Our spectroscopy reveals a grazing eclipse of the large outbursting disc. As the disc is significantly larger during outburst, it is unlikely that an eclipse will be detectable in quiescence. The relatively high accretion rate implied by the detection of outbursts, together with the large mass ratio, suggests that SBSS 1108+574 is still evolving towards its period minimum.en_US
dc.publisherOxford University Pressen_US
dc.rightsAtribución-NoComercial-SinDerivadas 3.0 España*
dc.subject.otherAccretion, accretion discsen_US
dc.subject.otherBinaries: closeen_US
dc.subject.otherStars: individual: SBSS 1108+574en_US
dc.subject.otherNovae, cataclysmic variablesen_US
dc.subject.otherWhite dwarfsen_US
dc.titleThe helium-rich cataclysmic variable SBSS 1108+574en_US

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