New findings based on long-term photometric observations of the eclipsing binary V471 Tauri

Details New findings based on long-term photometric observations of the eclipsing binary V471 Tauri New findings based on long-term photometric observations of the eclipsing binary V471 Tauri

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005mnras.360.1077i&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 360, Issue 3, pp. 1077-1084.

Astronomy and Astrophysics

Astronomy

11

Stars: Activity, Binaries: Eclipsing, Stars: Individual: V471 Tau, White Dwarfs

Scientific paper

The post-common envelope and pre-cataclysmic binary V471 Tau has been observed by the authors since 1973. At least a complete light curve in B and V bands and more than two eclipse timings were obtained in each year. All the available data published so far (including the authors') have been collected and analysed for the brightness and orbital period changes. The system brightened about 0.22 mag in both B and V bands more or less regularly up to 1997 and started to decrease afterwards. A search for periodicity of this variation yields a period longer than 85 yr. In addition to this long-period variation, a small amplitude of about 0.08 mag and short time-interval fluctuations on the mean brightness have been detected. The variations of the mean brightness have been discussed and plausible causes suggested. The changes of the apparent period have been attributed to a third body. Analysis of all the `observed-calculated' (O-C) data yields a period of 32.4 yr, with a semi-amplitude of 151 s and an eccentricity of 0.30 for the third-body orbit. For orbital inclinations greater than 34° the mass of the third body would possibly match to a brown dwarf. One of the most interesting features in the light curve of V471 Tau is the decrement of the eclipse depth with time. The depth of the eclipse in the B band has been decreased from 0.082 to 0.057 mag over 34 yr. Subtracting the variation of the depth due to the brightening of the red dwarf star, the actual variation in depth, originated from from the white dwarf, was found to be about 0.012 mag. This change in the brightness of the compact object has been attributed to the mass accretion from its primary component via thermally driven wind and/or flare-like events.

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