Abstract:
We present a detailed X-ray analysis and imaging of stellar coronae of five coronally connected eclipsing binaries,
namely, 44 Boo, DV Psc, ER Vul, XY UMa, and TX Cnc. Both components of these binaries are found to be
active. The X-ray light curves of detached and semidetached type systems show eclipsed-like features, whereas no
evidence for coronal eclipsing is shown by the contact type systems. The X-ray light curve of DV Psc shows the
O’Connell-like effect where the first maximum is found to be brighter than that of the second. Results of the
coronal imaging using three-dimensional deconvolution of X-ray light curves show the coronae of all these
binaries are either in the contact or over-contact configuration, with the primary being 1.7–4 times X-ray brighter
than its companion. In the current sample, a minimum of 30%–50% of total UV emission is found to originate from
the photosphere and positively correlated with the X-ray emission. X-ray spectra of these systems are well
explained by two-temperature plasma models. The temperature corresponding to cool and hot components of
plasma are found to be in the ranges of 0.25–0.64 and 0.9–1.1 keV, respectively. For the majority of binaries in the
sample, the phase-resolved X-ray spectral analysis shows the orbital modulation in X-ray luminosity and emission
measure corresponding to the hot component. A total of seven flaring events are also detected in the four systems
with the flare energy in the range of (1.95–27.0) × 1033 erg and loop length of the order of 109–11 cm.
