  We investigated dusty and dust-free gas dynamics for a radiation-driven
sub-pc scale outflow in an active galactic nucleus (AGN) associated with a
supermassive black hole $10^7 M_\odot$ and bolometric luminosity $10^{44}$ erg
s$^{-1}$ based on the two-dimensional radiation-hydrodynamic simulations. A
radiation-driven ``lotus-like'' multi-shell outflow is launched from the inner
part ($r \lesssim 0.04$ pc) of the geometrically thin disk, and it repeatedly
and steadily produces shocks as mass accretion continues through the disk to
the center. The shape of the dust sublimation radius is not spherical and
depends on the angle ($\theta$) from the disk plane, reflecting the
non-spherical radiation field and nonuniform dust-free gas. Moreover, we found
that the sublimation radius of $\theta \sim 20$-$60$ deg varies on a timescale
of several years. The ``inflow-induced outflow" contributes the obscuration of
the nucleus in the sub-parsec region. The column density of the dust-free gas
is $N_{\rm H} \gtrsim 10^{22}$ cm$^{-2}$ for $r \lesssim 0.04$ pc. Gases near
the disk plane ($\theta \lesssim 30$ degree) can be the origin of the
Compton-thick component, which was suggested by the recent X-ray observations
of AGNs. The dusty outflow from the sub-parsec region can be also a source of
material for the radiation-driven fountain for a larger scale.
