Abstract
We report on our spectroscopy of the short-period, 18th magnitude eclipsing binary NSV 12615. It shows a strong, broad and double-peaked Hα emission line, the width of which (3200±500 km s−1 FWZI) confirms that NSV 12615 is a cataclysmic variable and suggests it to be an SU UMa type system. We also detect its orbital motion. The semi-amplitude of the radial velocity variations (56±7 km s−1) suggests a higher (0.62–1.40 |$M_\odot$|) white dwarf mass than that estimated from the FWZI (0.2−0.4 |$M_\odot$|). We discuss the possible explanations for this result.
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