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≃104 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
∼5 kpc in ∼37 Myr for typical galactic parameters. The outflow
speed increases rapidly with the disc Eddington parameter Γ0(=κI/(2cGΣ)) for Γ0≥1.5. We find that the rotation speed of
the outflowing gas is ≲100 km s−1. The wind is confined in a
cone which mostly consist of low angular momentum gas lifted from the central
region.Comment: 10 pages, 11 figures, Accepted for publication in MNRA