  Evidently, low-luminosity active galactic nuclei LLAGNs comprise of inner
advective disk and outer geometrically thin disk. The wind is inevitable in
LLAGNs, mainly interpreted indirect way, also the evidences are growing for the
presence of wind in outer thin disk. We present a hydrodynamics HD model for
wind from outer thin disk where the main driver is the inner disk irradiation
(which is parameterized by a number $x$ in hydrostatic equilibrium equation
with a slightly unbalancing role). The model works for a low intense
irradiation or from a height $z_s$ in optically thin medium. We solve the model
equations in cylindrical coordinate along the $z$-axis for a given radius $r$
with assuming a tiny vertical speed $v_z$ ($\ll c_s$ sound speed). The sonic
point conditions assure an isobaric regime above the sonic height ($z^{max}$),
in addition from the height $z_f (\ll z^{max}$) the radial pressure gradient
also supports the fluid rotation, and both conjointly assure a wind ejection
from the $z^{max}$ with fluid speed. The $z^{max}$ increases with $x$, and
beyond a large $z^{max}$ (say $z^{max}_t$ corresponded to maximum $x$) there is
no physical solution. We start the computation from outer radius $r_o^{thin}$
to inner $r_{in}^{thin}$ with Bondi mass accretion rate $\dot{M}_{Bondi}$, to
explore the $r$ dependency of mass inflow rate $\dot{M}$ and wind properties.
We constrain the model by fixing $\dot{M}$ at $r_{in}^{thin}$ from the
observations of NGC 1097, and check the feasibility of model by comparing the
energetics with observed bolometric luminosity. The wind is an equatorial with
viewing angle $i>85$degree, and capable to generate red-/blue-shifted lines, it
would be a general characteristics for LLAGNs.
