  We investigate the Hoyle-Lyttleton accretion of dusty-gas for the case where
the central source is the black hole accretion disk. By solving the equation of
motion taking into account the radiation force which is attenuated by the dust
absorption, we reveal the steady structure of the flow around the central
object. We find that the mass accretion rate tends to increase with an increase
of the optical thickness of the flow and the gas can accrete even if the disk
luminosity exceeds the Eddington luminosity for the dusty-gas, since the
radiation force is weakened by the attenuation via the dust absorption. When
the gas flows in from the direction of the rotation axis for the disk with
${\Gamma}^{'}=3.0$, the accretion rate is about 93% of the Hoyle-Lyttleton
accretion rate if ${\tau}_{\rm{HL}}=3.3$ and zero for ${\tau}_{\rm{HL}}=1.0$,
where ${\Gamma}^{'}$ is the Eddington ratio for the dusty-gas and
${\tau}_{\rm{HL}}$ is the typical optical thickness of the Hoyle-Lyttleton
radius. Since the radiation flux in the direction of disk plane is small, the
radiation force tends not to prevent gas accretion from the direction near the
disk plane. For ${\tau}_{\rm{HL}}=3.3$ and ${\Gamma}^{'}=3.4$, although the
accretion is impossible in the case of ${\Theta}=0$, the accretion rate is 28%
of the Hoyle-Lyttleton one in the case of ${\Theta}=90$, where ${\Theta}$ is
the angle between the direction the gas is coming from and the rotation axis of
the disk. We also obtain relatively high accretion luminosity that is realized
when the accretion rate of the disk onto the BH is consistent with that via the
Hoyle-Lyttleton mechanism taking into account the effect of radiation. This
implies the intermediate-mass black holes moving in the dense dusty-gas are
identified as luminous objects in the infrared band.
