  In order to study the outflows from accretion disks, we solve the set of
hydrodynamic equations for accretion disks in the spherical coordinates
($r\theta\phi$) to obtain the explicit structure along the $\theta$ direction.
Using self-similar assumptions in the radial direction, we change the equations
to a set of ordinary differential equations (ODEs) about the
$\theta$-coordinate, which are then solved with symmetrical boundary conditions
in the equatorial plane, and the velocity field is obtained. The $\alpha$
viscosity prescription is applied and an advective factor $f$ is used to
simplify the energy equation.The results display thinner, quasi-Keplerian disks
for Shakura-Sunyaev Disks (SSDs) and thicker, sub-Keplerian disks for Advection
Dominated Accretion Flows (ADAFs) and slim disks, which are consistent with
previous popular analytical models. However, an inflow region and an outflow
region always exist, except when the viscosity parameter $\alpha$ is too large,
which supports the results of some recent numerical simulation works. Our
results indicate that the outflows should be common in various accretion disks
and may be stronger in slim disks, where both advection and radiation pressure
are dominant. We also present the structure dependence on the input parameters
and discuss their physical meanings. The caveats of this work and possible
improvements in the future are discussed.
