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We present a comprehensive study of three large long-duration flares detectedon an active M-dwarf binary EQ Peg using the Soft X-Ray Telescope of theAstroSat observatory. The peak X-ray luminosities of the flares in the 0.3 - 7keV band are found to be within ~5 - 10 x 10^{30} erg s^{-1}. The e-foldingrise- and decay-times of the flares are derived to be in the range of 3.4 - 11and 1.6 - 24 ks, respectively. Spectral analysis indicates the presence ofthree temperature corona with the first two plasma temperatures remain constantduring all the flares and the post-flare observation at ~3 and ~9 MK. The flaretemperature peaked at 26, 16, and 17 MK, which are 2, 1.3, and 1.4 times morethan the minimum value, respectively. The peak emission measures are found tobe 3.9 - 7.1 x 10^{53} cm^{-3}, whereas the abundances peaked at 0.16-0.26times the solar abundances. Using quasi-static loop modeling, we deriveloop-lengths for all the flares as 2.5+/-0.5 x 10^{11}, 2.0+/-0.5 x 10^{11},and 2.5+/-0.9 x 10^{11} cm, respectively. The density of the flaring plasma isestimated to be 4.2+/-0.8 x 10^{10}, 3.0+/-0.7 x 10^{10}, 2.2+/-0.8 x 10^{10}cm^{-3) for flares F1, F2, and F3, respectively. Whereas the magnetic field forall three flares is estimated to be <100 G. The estimated energies of all threeflares are ~10^{34-35} erg, putting them in a category of superflare. All threesuperflares are also found to be the longest duration flares ever observed onEQ Peg.

AstroSat observations of long-duration X-ray superflares on active M-dwarf binary EQ Peg