  We present results from simultaneous FUV and NUV observations of T-Tauri
stars (TTSs) in the Taurus molecular cloud with UVIT/AstroSat. This is the very
first UVIT study of TTSs. From the spectral energy distribution of TTSs from
FUV to near-IR, we show that classical TTSs (CTTSs) emit significantly higher
UV excess compared to weak-line TTSs (WTTSs). The equivalent black-body
temperatures corresponding to the UV excess in CTTSs ($>10^4$ K) are also found
to be relatively higher than that in WTTSs ($<9250$ K). From the UV excess, we
have re-classified two WTTSs (BS Tau, V836 Tau) as CTTSs, which has been
supported by the follow-up optical spectroscopic study using the Himalayan
Chandra Telescope (HCT), showing strong H$\alpha$ line emission. We find that
CTTSs show strong excess emission in both FUV ($>$10$^7$) and NUV ($>$10$^3$)
bands, while WTTSs show strong excess only in the FUV ($\lesssim$10$^5$),
suggesting that excess emission in NUV can be used as a tool to classify the
TTSs. We also find a linear correlation between UV luminosity (a primary
indicator of mass accretion) and H$\alpha$ luminosity (a secondary indicator of
mass accretion) with a slope of 1.20$\pm$0.22 and intercept of 2.16$\pm$0.70.
