Subparsec-scale dynamics of a dusty gas disk exposed to anisotropic AGN
  radiation with frequency-dependent radiative transfer
  We explore the gas dynamics near the dust sublimation radius of active
galactic nucleus (AGN). For the purpose, we perform axisymmetric radiation
hydrodynamic simulations of a dusty gas disk of radius $\approx 1\,\mathrm{pc}$
around a supermassive black hole of mass $10^{7}\,\mathrm{M_{\odot}}$ taking
into account (1) anisotropic radiation of accretion disk, (2) X-ray heating by
corona, (3) radiative transfer of infrared (IR) photons reemitted by dust, (4)
frequency dependency of direct and IR radiations, and (5) separate temperatures
for gas and dust. As a result, we find that for Eddington ratio $\approx 0.77$,
a nearly neutral, dense ($\approx 10^{6\operatorname{-}8}\;\mathrm{cm^{-3}}$),
geometrically-thin ($h/r<0.06$) disk forms with a high velocity ($\approx 200
\sim 3000\;\mathrm{km/s}$) dusty outflow launched from the disk surface. The
disk temperature is determined by the balance between X-ray heating and various
cooling, and the disk is almost supported by thermal pressure. Contrary to
\citet{krolik07:_agn}, the radiation pressure by IR photons is not effective to
thicken the disk, but rather compresses it. Thus, it seems difficult for a
radiation-supported, geometrically-thick, obscuring torus to form near the dust
sublimation radius as far as the Eddington ratio is high ($\sim 1$). The mass
outflow rate is $0.05$-$0.1\;\mathrm{M_{\odot}}/\mathrm{yr}$ and the column
density of the outflow is $N_{\mathrm{H}}\lesssim 10^{21}\;\mathrm{cm^{-2}}$.
To explain observed type-II AGN fraction, it is required that outflow gas is
extended to larger radii ($r\gtrsim 10\;\mathrm{pc}$) or that a denser dusty
wind is launched from smaller radii ($r\sim 10^{4}\;R_{g}$).
