The late flare in tidal disruption events due to the interaction of disk
  wind with dusty torus
  A late (t $\sim$ 1,500 days) multi-wavelength (UV, optical, IR, and X-ray)
flare was found in PS1-10adi, a tidal disruption event (TDE) candidate that
took place in an active galactic nucleus (AGN). TDEs usually involve
super-Eddington accretion, which drives fast mass outflow (disk wind). So here
we explore a possible scenario that such a flare might be produced by the
interaction of the disk wind with a dusty torus for TDEs in AGN. Due to the
high velocity of the disk wind, strong shocks will emerge and convert the bulk
of the kinetic energy of the disk wind to radiation. We calculate the dynamics
and then predict the associated radiation signatures, taking into account the
widths of the wind and torus. We compare our model with the bolometric light
curve of the late flare in PS1-10adi constructed from observations. We find
from our modeling that the disk wind has a total kinetic energy of about
$10^{51}$ erg and a velocity of 0.1 c (i.e., a mass of 0.3 $M_{\odot}$); the
gas number density of the clouds in the torus is $3\times 10^{7}$ $\rm
cm^{-3}$. Observation of such a late flare can be an evidence of the disk wind
in TDEs and can be used as a tool to explore the nuclear environment of the
host.
