  The paper demonstrates the spectroscopic and photometric capabilities of the
Ultra-Violet Imaging Telescope (UVIT) to study T-Tauri stars (TTSs). We present
the first UVIT/Far-UV spectrum of a TTS, TW Hya. Based on C IV line luminosity,
we estimated accretion luminosity (0.1 $L_\odot$) and mass accretion rate (2.2
$\times$ $10^{-8} M_\odot /yr$) of TW Hya, and compared these values with the
accretion luminosity (0.03 $L_\odot$) and mass accretion rate (0.6 $\times$
$10^{-8} M_\odot /yr$) derived from spectral energy distribution (SED). From
the SED, we derive best-fitted parameters for TW Hya: $T_{eff}$ = 3900$\pm$50
K, radius = 1.2$\pm$0.03 $R_\odot$, $\mathrm{log}\, g = 4.0$ and equivalent
black-body temperatures corresponding to accretion luminosity as 14100$\pm$25
K. The parameters of TW Hya derived from UVIT observations were found to be
matched well with the literature. Comparison with IUE spectra also suggests
that UVIT can be used to study the spectroscopic variability of young stars.
This study proposes leveraging the FUV spectroscopic capabilities of UVIT to
contribute to the advancement of upcoming UV spectroscopic missions, including
the Indian Spectroscopic Imaging Space Telescope (INSIST).
