  $\require{mediawiki-texvc}$ We study accretion disk emission from eight
Seyfert $1 - 1.5$ active galactic nuclei (AGN) using far ultra-violet
($1300-1800$ ${\AA}$) slit-less grating spectra acquired with AstroSat/UVIT. We
correct for the Galactic and intrinsic extinction, contamination from the host
galaxies, narrow and broad-line regions, Fe II emission and Balmer continuum,
and derive the intrinsic continua. We use HST COS/FOS spectra to account for
the emission/absorption lines in the low-resolution UVIT spectra. We find
generally redder power-law ($f_\nu \propto \nu^{\alpha}$) slopes ($\alpha \sim
-1.1 - 0.3$) in the far UV band than predicted by the standard accretion disk
model in the optical/UV band. We fit accretion disk models such as the
multi-temperature disk blackbody ($\texttt{DISKBB}$) and relativistic disk
($\texttt{ZKERRBB}$, $\texttt{OPTXAGNF}$) models to the observed intrinsic
continuum emission. We measure the inner disk temperatures using the
$\texttt{DISKBB}$ model for seven AGN. These temperatures in the range $\sim
3.6-5.8$ eV are lower than the peak temperatures predicted for standard disks
around maximally spinning super-massive black holes accreting at Eddington
rates. The inner disks in two AGN, NGC 7469 and Mrk 352, appear to be truncated
at $\sim 35-125r_{g}$ and $50-135r_{g}$, respectively. While our results show
that the intrinsic FUV emission from the AGN are consistent with the standard
disks, it is possible that UV continua may be affected by the presence of soft
X-ray excess emission, X-ray reprocessing, and thermal Comptonisation in the
hot corona. Joint spectral modeling of simultaneously acquired UV/X-ray data
may be necessary to further investigate the nature of accretion disks in AGN.
