  Many astrophysical sources, e.g., cataclysmic variables, X-ray binaries,
active galactic nuclei, exhibit a wind outflow, when they reveal a multicolor
blackbody spectrum, hence harboring a geometrically thin Keplerian accretion
disk. Unlike an advective disk, in the thin disk, the physical environment,
like, emission line, external heating, is expected to play a key role to drive
the wind outflow. We show the wind outflow in a thin disk attributing a disk
irradiation effect, probably from the inner to outer disks. We solve the set of
steady, axisymmetric disk model equations in cylindrical coordinates along the
vertical direction for a given launching radius $(r)$ from the midplane,
introducing irradiation as a parameter. We obtain an acceleration solution, for
a finite irradiation in the presence of a fixed but tiny initial vertical
velocity (hence thin disk properties practically do not alter) at the midplane,
upto a maximum height ($z^{max}$). We find that wind outflow mainly occurs from
the outer region of the disk and its density decreases with increasing
launching radius, and for a given launching radius with increasing ejection
height. Wind power decreases with increasing ejection height. For $z^{max} <
2r$, wind outflow is ejected tangentially (or parallel to the disk midplane) in
all directions with the fluid speed same as the azimuthal speed. This confirms
mainly, for low mass X-ray binaries, (a) wind outflow should be preferentially
observed in high-inclination sources, (b) the expectation of red and blue
shifted absorption lines.
