Relativistic accretion disc in tidal disruption events
  We construct a time-dependent relativistic accretion model for tidal
disruption events (TDEs) with an $\alpha-$viscosity and the pressure dominated
by gas pressure. We also include the mass fallback rate $\dot{M}_f$ for both
full and partial disruption TDEs, and assume that the infalling debris forms a
seed disc in time $t_c$, which evolves due to the mass addition from the
infalling debris and the mass loss via accretion onto the black hole. Besides,
we derive an explicit form for the disc height that depends on the angular
momentum parameter in the disc. We show that the surface density of the disc
increases at an initial time due to mass addition, and then decreases as the
mass fallback rate decreases, which results in a decrease in the disc mass
$M_{\rm d}$ with a late-time evolution of $M_{\rm d} \propto t^{-1.05}$ and
$M_{\rm d} \propto t^{-1.38}$ for full and partial disruption TDEs
respectively, where $t$ is the time parameter. The bolometric luminosity $L$
shows a rise and decline that follows a power-law at late times given by $L
\propto t^{-1.8}$ and $L \propto t^{-2.3}$ for full and partial disruption TDEs
respectively. Our obtained luminosity declines faster than the luminosity
inferred using $L \propto \dot{M}_f$. We also compute the light curves in
various spectral bands.
