Periods and Quasiperiods in the Cataclysmic Variable BZ Camelopardalis

Details Periods and Quasiperiods in the Cataclysmic Variable BZ Camelopardalis Periods and Quasiperiods in the Cataclysmic Variable BZ Camelopardalis

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aj....111.2422p&link_type=abstract

Astronomical Journal v.111, p.2422

Astronomy and Astrophysics

Astronomy

16

Cataclysmic Variables, Stars: Individual: Bz Camelopardalis, Stars: Oscillations

Scientific paper

We report a study of spectroscopic and photometric variations in the cataclysmic variable BZ Camelopardalis. The emission lines move in radial velocity with an underlying period of 0.1533 d, which we take to be the orbital period. A more precise measurement, combining spectroscopic and photometric data, suggests Porb=O. 153693(7) d. The line profiles are characterized by titanic struggles between emission and absorption, roughly resembling the components of a "P Cygni" profile; but the motions of these components do not repeat on the orbital period. The lines probably originate partly in the binary system and partly in an outflowing stellar wind. The light curves are very complex. Precise identification of periods is hampered by the low and variable amplitudes (semiamplitudes <0.03 mag), but the data suggest the existence of transient signals below and above the orbital frequency. Other possible signals appear near low harmonics of the orbital frequency. It is possible that these represent an unusual incarnation of "superhumps."

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