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2013MNRAS.431..372C - Mon. Not. R. Astron. Soc., 431, 372-382 (2013/May-1)
The helium-rich cataclysmic variable SBSS 1108+574.
CARTER P.J., STEEGHS D., DE MIGUEL E., GOFF W., KOFF R.A., KRAJCI T., MARSH T.R., GANSICKE B.T., BREEDT E., GROOT P.J., NELEMANS G., ROELOFS G.H.A., RAU A., KOESTER D. and KUPFER T.
Abstract (from CDS):
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.
Abstract Copyright: © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2013)
Journal keyword(s): accretion, accretion discs - binaries: close - stars: individual: SBSS 1108+574 - novae, cataclysmic variables - white dwarfs
Simbad objects: 10
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