Simulation of radiation driven wind from disc galaxies
  We present 2-D hydrodynamic simulation of rotating galactic winds driven by
radiation. We study the structure and dynamics of the cool and/or warm
component($T \simeq 10^4$ K) which is mixed with dust. We have taken into
account the total gravity of a galactic system that consists of a disc, a bulge
and a dark matter halo. We find that the combined effect of gravity and
radiation pressure from a realistic disc drives the gas away to a distance of
$\sim 5$ kpc in $\sim 37$ Myr for typical galactic parameters. The outflow
speed increases rapidly with the disc Eddington parameter $\Gamma_0(=\kappa
I/(2 c G \Sigma)$) for $\Gamma_0 \ge 1.5$. We find that the rotation speed of
the outflowing gas is $\lesssim 100$ km s$^{-1}$. The wind is confined in a
cone which mostly consist of low angular momentum gas lifted from the central
region.
