A study of an X-ray flare on the solar analogue V895 Tau

Using observations with XMM-Newton, we study the characteristics of a flare emanating from a solar analogous V895 Tau. At the peak of the flare, its luminosity reached 3.3×1030ergs−1, which is ∼ 600 times more energetic than the X10 class flare on the Sun. The quiescent state corona of V895 Tau is depicted by a two-temperature plasma model with temperatures of 3.9 and 11 MK. The flare’s evolution was carefully scrutinized through time-resolved X-ray spectroscopy, unveiling the variations in temperature, emission measure, abundance and luminosity during the flare. The temperature peaked at 36.1 MK, which is approximately four times higher than the pre-flare temperature. Employing a hydrodynamic loop model, we have estimated the half length of the flaring loop to be 5.9×1010 cm. Using the loop scaling laws, other loop parameters like density, pressure, volume, and minimum magnetic field are also estimated, and are found to be similar to those of other flares from similar type of stars. •Strongest X-ray superflare on solar analogue V895 Tau detected•Energy release during flare is 1.6×1034 erg•The quiescent corona is explained by a two-temperature plasma at 3.9 and 11 MK•The loop length of flaring plasma is 0.7 times the stellar radius•The coronal abundances increase by three times during the flare peak