PERIODS AND QUASI-PERIODS IN THE CATACLYSMIC VARIABLE BZ CAMELOPARDALIS

We report a study of spectroscopic and photometric variations in the c ataclysmic variable BZ Camelopardalis. The emission lines move in radi al velocity with an underlying period of 0.1533 d, which we take to be the orbital period. A more precise measurement, combining spectroscop ic and photometric data, suggests P-orb=0.153693(7) d. The line profil es are characterized by titanic struggles between emission and absorpt ion, roughly resembling the components of a ''P Cygni'' profile; but t he motions of these components do not repeat un the orbital period. Th e lines probably originate partly in the binary system and partly in a n outflowing stellar wind. The light curves are very complex. Precise identification of periods is hampered by the low and variable amplitud es (semiamplitudes <0.03 mag), but the data suggest the existence of t ransient signals below and above the orbital frequency. Other possible signals appear near low harmonics of the orbital frequency. It is pos sible thar these represent an unusual incantation of ''superhumps.'' ( C) 1995 American Astronomical Society.