Dynamical masses of a nova-like variable on the edge of the period gap

TL;DR

This study provides the first dynamical measurements of binary parameters for an eclipsing SW Sextantis star during a low state, revealing detailed stellar masses, spectral types, and the first detection of a DAB white dwarf in a cataclysmic variable.

Contribution

It offers the first dynamical determination of binary parameters for an eclipsing SW Sextantis star in a low state, including white dwarf and secondary star masses and spectral properties.

Findings

White dwarf mass: 0.87 ± 0.09 M_sun

Secondary star mass: 0.47 ± 0.05 M_sun

First detection of a DAB white dwarf in a CV

Abstract

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 $\pm$ 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 $\pm$ 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 M$_1 = 0.87 \pm 0.09$ M$_\odot$ and M$_2 = 0.47 \pm 0.05$ M$_\odot$ for the white dwarf and the M dwarf, respectively, and an inclination of the orbital plane of $i \approx 79^\mathrm{o}$. A radius of $0.0103 \pm 0.0007$ R$_\odot$ is obtained for the white dwarf. The secondary star in HS 0220+0603 is likely too cool and undersized for its mass.