  Winds play a significant role in active galactic nuclei feedback process.
Previous simulations studying winds only focus on a small dynamical range.
Therefore, it is unknown how far the winds can go and what the properties of
the winds will be if they can move to large radii. We perform simulations to
study the large scale dynamics of winds driven by line force. We find that the
properties of the winds depend on both black hole mass ($M_{BH}$) and accretion
disk luminosity. When the accretion disk luminosity is $0.6L_{edd}$ ($L_{edd}$
being Eddington luminosity), independent of $M_{BH}$, the winds have kinetic
energy flux exceeding $1\% L_{edd}$ and can escape from the black hole
potential. For the case with the accretion disk luminosity equaling
0.3$L_{edd}$, the strength of the winds decreases with the decrease of
$M_{BH}$. If $M_{BH}$ decreases from $10^9$ to $10^6$ solar mass ($M_\odot$),
the winds kinetic energy flux decreases from $\sim 0.01 L_{edd}$ to $ \sim
10^{-6} L_{edd}$. In case of $M_{BH}\geq 10^7 M_\odot$, winds can escape from
black hole potential. In the case of $M_{BH}=10^6 M_\odot$, the winds can not
escape. We find that for the ultra-fast winds observed in hard X-ray bands
(\citealt{Gofford et al. 2015}), the observed dependence of the mass flux and
the kinetic energy flux on accretion disk luminosity can be well produced by
line force driven winds model. We also find that the properties of the
ultra-fast winds observed in soft X-ray bands can be explained by the line
force driven winds model.
