We present the results of axisymmetric time-dependent hydrodynamic calculations of line-driven winds from accretion disks in active galactic nuclei ( AGN ) .
We assume the disk is flat , Keplerian , geometrically thin , and optically thick , radiating according to the \alpha -disk prescription .
The central engine of the AGN is a source of both ionizing X-rays and wind-driving ultraviolet ( UV ) photons .
To calculate the radiation force , we take into account radiation from the disk and the central engine .
The gas temperature and ionization state in the wind are calculated self-consistently from the photoionization and heating rate of the central engine .

We find that a disk accreting onto a 10 ^ { 8 } ~ { } M _ { \odot } black hole at the rate of 1.8 ~ { } M _ { \odot } yr ^ { -1 } can launch a wind at \sim 10 ^ { 16 } cm from the central engine .
The X-rays from the central object are significantly attenuated by the disk atmosphere so they can not prevent the local disk radiation from pushing matter away from the disk .
However in the supersonic portion of the flow high above the disk , the X-rays can overionize the gas and decrease the wind terminal velocity .
For a reasonable X-ray opacity , e.g. , \kappa _ { X } = 40 ~ { } g ^ { -1 } ~ { } cm ^ { 2 } , the disk wind can be accelerated by the central UV radiation to velocities of up to 15000 km~ { } s ^ { -1 } at a distance of \sim 10 ^ { 17 } cm from the central engine .
The covering factor of the disk wind is \sim 0.2 .
The wind is unsteady and consists of an opaque , slow vertical flow near the disk that is bounded on the polar side by a high-velocity stream .
A typical column density through the fast stream is a few 10 ^ { 23 } ~ { } cm ^ { -2 } so the stream is optically thin to the UV radiation .
This low column density is precisely why gas can be accelerated to high velocities .
The fast stream contributes nearly 100 % to the total wind mass loss rate of 0.5 ~ { } M _ { \odot } yr ^ { -1 } .