Dynamics of accretion and winds in tidal disruption events
  We have constructed self-similar models of a time-dependent accretion disk in
both sub and super-Eddington phases with wind outflows for tidal disruption
events (TDEs). The physical input parameters are the black hole (BH) mass
$M_{\bullet}$, specific orbital energy $E$ and angular momentum $J$, star mass
$M_{\star}$ and radius $R_{\star}$. We consider the sub-Eddington phase to be
total pressure (model A1) and gas pressure (model A2) dominated. In contrast,
the super-Eddington phase is dominated by radiation pressure (model B) with
Thomson opacity. We derive the viscosity prescribed by the stress tensor,
$\Pi_{r\phi}\propto \Sigma_d^b r^d$ where $\Sigma_d$ is the surface density of
the disk, $r$ is the radius and $b$ and $d$ are constants. The specific choice
of radiative or $\alpha$ viscosity is motivated, and its parameters are decided
by the expected disk luminosity and evolution time scale being in the observed
range. The disk evolves due to mass loss by accretion onto the black hole and
outflowing wind, and mass gain by fallback of the debris; this results in an
increasing outer radius. We have simulated the luminosity profile for both sub
and super-Eddington disks. As an illustrative example, we fit our models to the
observations in X-ray, UV, and Optical of four TDE events and deduce the
physical parameters above.
