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29 March 2024
 
  » arxiv » astro-ph/0410223

 Article overview


HS2331+3905: The cataclysmic variable that has it all
S. Araujo-Betancor ; B.T. Gaensicke ; H.-J. Hagen ; T.R. Marsh ; E.T. Harlaftis ; J. Thorstensen ; R.E. Fried ; P. Schmeer ; D. Engels ;
Date 8 Oct 2004
Journal Astron.Astrophys. 430 (2005) 629
Subject astro-ph
AbstractWe report detailed follow-up observations of the cataclysmic variable HS2331+3905, identified as an emission-line object in the Hamburg Quasar Survey. An orbital period of 81.08min is unambiguously determined from the detection of eclipses in the light curves of HS2331+3905. A second photometric period is consistently detected at P~83.38min, ~2.8% longer than the orbital period, which we tentatively relate to the presence of permanent superhumps. High time resolution photometry exhibits short-timescale variability on time scales of 5-6min which we interpret as non-radial white dwarf pulsations, as well as a coherent signal at 1.12min, which is likely to be the white dwarf spin period. A large-amplitude quasi-sinusoidal radial velocity modulation of the Balmer and Helium lines with a period ~3.5h is persistently detected throughout three seasons of time-resolved spectroscopy. However, this spectroscopic period, which is in no way related to the orbital period, is not strictly coherent but drifts in period and/or phase on time scales of a few days. Modeling the far-ultraviolet to infrared spectral energy distribution of HS2331+3905, we determine a white dwarf temperature of Teff=10500K (assuming Mwd=0.6Msun), close to the ZZ Ceti instability strip of single white dwarfs. The spectral model implies a distance of d=90+-15pc, and a low value for the distance is supported by the large proper motion of the system, mu=0.14"/yr. The non-detection of molecular bands and the low J, H, and K fluxes of HS2331+3905 make this object a very likely candidate for a brown-dwarf donor.
Source arXiv, astro-ph/0410223
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