2015/06/09 by Rodríguez-Gil, P., Shahbaz, T., Marsh, T. R. +12
#FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR)
paper · doi:10.48550/arxiv.1506.02980
We present the first dynamical determination of the binary parameters of an eclipsing SW Sextantis star in the 3-4 hour orbital period range during a low state. We obtained time-resolved optical spectroscopy and photometry of HS 0220+0603 during its 2004-2005 low brightness state, as revealed in the combined SMARTS, IAC80 and M1 Group long-term optical light curve. The optical spectra taken during primary eclipse reveal a secondary star spectral type of M5.5 ± 0.5 as derived from molecular band-head indices. The spectra also provide the first detection of a DAB white dwarf in a cataclysmic variable. By modelling its optical spectrum we estimate a white dwarf temperature of 30000 ± 5000 K. By combining the results of modelling the white dwarf eclipse from ULTRACAM light curves with those obtained by simultaneously fitting the emission- and absorption-line radial velocity curves and I-band ellipsoidal light curves, we measure the stellar masses to be M1 = 0.87 ± 0.09 M_\odot and M2 = 0.47 ± 0.05 M_\odot for the white dwarf and the M dwarf, respectively, and an inclination of the orbital plane of i ≈ 79o. A radius of 0.0103 ± 0.0007 R_\odot is obtained for the white dwarf. The secondary star in HS 0220+0603 is likely too cool and undersized for its mass.