Abstract
Coronal emission exhibited by the chromospherically active binaries is important to understand the underlying mechanism. We report the X-ray spectral studies of an RS CVn source CF Tuc using XMM-Newton archival data. The light curve was found to be steady with no flaring activity and the source was in a quiescent X-ray emission state. The source spectrum can be explained by a three-component thin plasma model with temperatures ∼ 0.26 keV, ∼1.01 keV, and ∼2.14 keV using EPIC MOS and pn data. We found that the source exhibits low abundance Z = 0.1−0.2 Z⊙, well in agreement with previous studies. Based on the RGS spectral fits of OVII triplets, we estimated the temperature to be about 1−2 × 106 K and density ne= 1−2 × 1010 cm−3 of the coronal emission region during the quiescent state.
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