  We present an analysis of seven flares detected from five RS CVn-type
binaries (UZ Lib, \sigma Gem, \lambda And, V711 Tau and EI Eri) observed with
XMM-Newton observatory. The quiescent state X-ray luminosities in the energy
band of 0.3-10.0 keV of these stars were found to be 10^{30.7-30.9} erg/s. The
exponential decay time in all the sample of flares range from ~ 1 to 8 hrs. The
luminosity at peak of the flares in the energy band of 0.3-10.0 keV were found
to be in the range of 10^{30.8} - 10^{31.8} erg/s. The great sensitivity of the
XMM-EPIC instruments allowed us to perform time resolved spectral analysis
during the flares and also in the subsquent quiescent phases. The derived metal
abundances of coronal plasma were found to vary during the flares observed from
\sigma Gem, V771 Tau and EI Eri. In these flares elemental abundances found to
be enhanced by factors of ~ 1.3-1.5 to the quiescent states. In most of the
flares, the peak temperature was found to be more than 100 MK whereas emission
measure increased by factors of 1.5 - 5.5. Significant sustained heating was
present in the majority of flares. The loop lengths (L) derived for flaring
structure were found to be of the order of 10^{10 -11} cm and are smaller than
the stellar radii (R*) i.e. L/R* \lesssim 1. The flare from \sigma Gem showed a
high and variable absorption column density during the flare.
