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Time‐Resolved Spectroscopy and Photometry of CT Serpentis and V825 Herculis

Time‐resolved spectroscopy and photometry of two cataclysmic variables (CVs) are presented. A radial velocity study shows CT Ser (Nova Ser 1948) has an orbital period of 0.195 ± 0.002 days. Its light curve shows only erratic flickering. A radial velocity study shows that V825 Her (PG 1717+413) has an orbital period of 0.206 ± 0.002 days. This CV’s spectrum is similar to that of a dwarf nova in outburst, or an old nova: the long‐term light curve shows only small, “stunted” outbursts, so it is likely to be a luminous nova‐like CV, similar to a dwarf nova stuck in outburst all the time. We use time‐resolved photometry to discover quasi‐periodic oscillations (QPOs), with periods between 15 and 24 minutes, not unlike those seen in other luminous CVs.