| Abstract : | The coronae of cool stars consists primarily of a magnetically driven hot plasma that emits X-rays. The interaction between the coronae of two cool stars can be studied via studying semi-detached binaries, which consists of two active late-type stars. We present the detailed X-ray study of such a semi-detached eclipsing binary, DV Psc using the XMM-Newton data spanning around two full cycles of period for this binary. We found, the quiescent state of DV Psc consists of two-temperature plasma with hot and cool temperature components of 0.25 and 1.0 keV, respectively. The time-resolved spectroscopy shows no significant variability of these temperature components with phase of binary. However, emission measures and coronal abundance shows variability at 99% and 68% confidence level. The coronal eclipsing is found, with suppression of about 20% during the secondary eclipse from the mean value of X-ray flux. Further, the system shows out of eclipse variability, which is modelled using 3D-deconvolution of phase folded X-ray lightcurve. The model shows X-ray emitting regions are situated at high latitudes. The simultaneous UV lightcurve shows a positive correlation with X-ray lightcurve. Two flaring episodes are also been observed. The flare temperatures are found to be around 3 keV for both the flares. Our results show that, coronae of both the components of DV PSc are X-ray active and shares a physical contact. |
