期刊
ASTROPHYSICAL JOURNAL
卷 877, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab19c3
关键词
binaries: eclipsing; stars: chromospheres; stars: flare; stars: individual (DV Psc); starspots
资金
- Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
- Key Laboratory of Optical Astronomy, NAOC, CAS
- National Natural Science Foundation of China (NSFC) [U1631236, U1431114]
- Chinese Academy of Sciences (CAS) [U1631236, U1431114]
- NSFC [11203005, 10373023]
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 degrees and 270 degrees. We obtained its starspot cycles with periods of 3.60 +/- 0.03 yr and 3.42 +/- 0.02 yr at about 90 degrees and 270 degrees, 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 10(24) 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 H-alpha, line and small self-reversal emissions of the Ca II IRT lines.
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