| Abstract : | Flares are sudden explosive release of magnetic energy stored in magnetic coronal loops due to the magnetic reconnection process. Young active stars show enhanced level of flaring activity due to their high rotation rate. We present an analysis of one of the strongest X-ray flare observed by XMM-Newton satellite on 02/01/2011 in AB Dor. This flare was found to last for ~1 hr with peak X-ray luminosity and peak temperature of ~3.21*10^30 erg/s and ~6.47*10^7 K, respectively. whereas, the quiescent state coronae of AB Dor was represented by a three temperature plasma with temperatures of 0.33*10^7 K, 1.12*10^7 K, and 2.49*10^7 K. The time-resolved X-ray spectroscopy of the flare shows the variable nature of the temperature, the emission measure, and the abundance. Using the high resolution X-ray spectroscopy, we found that the abundances during the flare were increased and show the inverse FIP effect i.e. the depletion in coronal abundance of elements like Fe, Mg, and Si (low FIP) that are ionized in the chromosphere relative to those that are neutral (high FIP). By employing the hydrodynamic loop model, we derive the semi-loop length of the flare is 1.4x10^10 cm. |
