Abstract

Taking advantage of the high sensitivity of XMM-EPIC instruments, we perform time resolved spectral analysis during the flares from mainsequence (MS) and evolved cool stars. The temporal and spectral characteristics of observed flares in stars on MS and giant branch are found to be similar to solar arced flares. Loop length derived for the flaring structure are much less than the stellar radius (length L < R _★) for MS and evolved late-type stars. However, for most of the pre-mainsequence (PMS) stars loop length is found to be much larger than the stellar radius (length L ≥ R _★). The temperatures at flare peak are often very high, with most of the flares in the sample showing temperatures in excess of 100 MK.