Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.264..132h&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Vol. 264, NO. 1/SEP1, P. 132, 1993
Astronomy and Astrophysics
Astronomy
38
Accretion, Accretion Discs - Celestial Mechanics, Stellar Dynamics - Stars: Individual: Tv Col - Novae, Cataclysmic Variables
Scientific paper
I present six nights of simultaneous optical photometry and spectroscopy aimed at observing the four periodicities of TV Col. The 32-min white dwarf spin period (known from the X-ray band) is not convincingly detected in the optical. The 5.5-h orbital period is manifest both photometrically and in the emission-line radial velocities. The emission lines show disc emission with a superimposed S-wave. Near orbital phase 0.8, the S-wave is at inferior conjunction, the photometric variation is at minimum, there is absorption in the line centres and we see X-ray dips. All these findings suggest that the rim of the disc is thickened at this location.
The 4-d and 5.2-h cycles dominate the continuum variations but do not change the emission-line profiles. These modulations are not absolutely coherent. One photometric data set suggests that the optical eclipse (of the near part of the accretion disc only) has a depth independent of 4-d!5.2-h phase and source brightness. Other photometry is inconclusive owing to the shallowness of the eclipses and the small amplitude of the brightness variations. I discuss the origin of the extra modulations, concluding that they are probably caused by an accretion disc precessing with a 4-d retrograde cycle and interacting tidally with the secondary to produce the 5.2-h modulation. This phenomenon (possibly also occurring in TT Ari) has similarities to SU UMa stars in superoutburst, but the SU UMa mechanism cannot be applied directly to TV Col.
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