  We perform two-dimensional hydrodynamical simulations of slowly rotating
accretion flows in the region of $ 0.01-7\, \mathrm{pc} $ around a supermassive
black holes with $ M_\mathrm{BH} = 10^{8} M_{\odot} $. The accretion flow is
irradiated by the photons from the central active galactic nucleus (AGN). In
addition to the direct radiation from the AGN, we have also included the
"re-radiation", i.e., the locally produced radiation by Thomson scattering,
line and bremsstrahlung radiation. Compare to our previous work, we have
improved the calculation of radiation force due to the Thomson scattering of
X-ray photons from the central AGN. We find that this improvement can
significantly increase the mass flux and velocity of outflow. We have compared
the properties of outflow --- including mass outflow rate, velocity, and
kinetic luminosity of outflow --- in our simulation with the observed
properties of outflow in AGNs and found that they are in good consistency. This
implies that the combination of line and re-radiation forces is the possible
origin of observed outflow in luminous AGNs.
