  We present observations of the active M-dwarf binary AT Mic (dM4.5e+dM4.5e)
obtained with the orbital observatory AstroSat. During 20 ks of observations,
in the far ultraviolet ($130-180$ nm) and soft X-ray ($0.3-7$ keV) spectral
ranges, we detected both quiescent emission and at least five flares on
different components of the binary. The X-ray flares were typically longer than
and delayed (by $5-6$ min) with respect to their ultraviolet counterparts, in
agreement with the Neupert effect. Using X-ray spectral fits, we have estimated
the parameters of the emitting plasma. The results indicate the presence of a
hot multi-thermal corona with the average temperatures in the range of $\sim
7-15$ MK and the emission measure of $\sim (2.9-4.5)\times 10^{52}$
$\textrm{cm}^{-3}$; both the temperature and the emission measure increased
during the flares. The estimated abundance of heavy elements in the corona of
AT Mic is considerably lower than at the Sun ($\sim 0.18-0.34$ of the solar
photospheric value); the coronal abundance increased during the flares due to
chromospheric evaporation. The detected flares had the energies of $\sim
10^{31}-10^{32}$ erg; the energy-duration relations indicate the presence of
magnetic fields stronger than in typical solar flares.
