| In this talk I will present X-ray flares observed from the Solar analogue at different evolutionary stages. The great sensitivity of XMM-Newton and Chandra allows us to determine the physical parameters (e.g. loop length, temperature etc.) of the flaring plasma. The temporal and spectral characteristics of observed flares in these stars are found to be similar to solar arced flares. Recent results show that loop length derived for the flaring structure are much less than the stellar radius for main-sequence and evolved late-type stars. However, for most of the pre-mainsequence stars loop length is found to be much larger than the stellar radius.