Astrophys. J., 877, 75-75 (2019/June-1)
Magnetic activity and orbital period study for the short-period RS CVn-type eclipsing binary DV Psc.
PI Q.-F., ZHANG L.-Y., BI S.-L., HAN X.L., LU H.-P., YUE Q., LONG L. and YAN Y.
Abstract (from CDS):
Using 27 sets of new multiband photometry light curves acquired from our long-term photometric campaign carried out in the last 5 yr and high-resolution spectroscopic data from seven nights, we analyzed the physical mechanisms of period variation, starspot cycle, optical flares, and chromospheric activities of the eclipsing binary DV Psc. Our updated O - C diagram covering a period of approximately 20 yr shows an oscillation in its orbital period. This variations might be caused by a third body with an orbital period of 14.58 ± 0.28 yr. There are two active regions of starspots at longitude belts of about 90° and 270°. We obtained its starspot cycles with periods of 3.60 ± 0.03 yr and 3.42 ± 0.02 yr at about 90° and 270°, respectively. Moreover, the magnitude difference of Max. I-Max. II shows cyclic oscillation of 5.15 ± 0.01 yr. During our decade long photometric campaign, we observed DV Psc a total of 326.4 hr, detected 18 outbursts (12 of them have never been reported) with flare energies in the range of (6.62-1106.85) x 1024 J. The slope of the relationship between the phase of the max flare and spots is 0.842 ± 0.083, implying a correlation between spots and flares. We discovered evidence for a correlation between the rotation period and the activity cycle for the short-period eclipsing binaries. Our high-resolution spectroscopic observations of DV Psc show obvious emissions above continuum in the Hα line and small self-reversal emissions of the Ca II IRT lines.
© 2019. The American Astronomical Society.
binaries: eclipsing - stars: chromospheres - stars: flare - stars: individual: DV Psc - starspots
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