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 Γ′ = 3.0, the accretion rate is about $93\%$ of the Hoyle–Lyttleton accretion rate if τHL = 3.3 and zero for τHL = 1.0, where Γ′ is the Eddington ratio for the dusty gas and τHL 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 τHL = 3.3 and Γ′ = 3.4, although the accretion is impossible in the case of Θ = 0°, the accretion rate is $28\%$ of the Hoyle–Lyttleton one in the case of Θ = 90°, where Θ 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 on to the BH is consistent with that via the Hoyle–Lyttleton mechanism taking into account the effect of radiation. This implies that the intermediate-mass black holes moving in the dense dusty gas are identified as luminous objects in the infrared band.

中文翻译：

---

Hoyle-Lyttleton 吸积到具有超爱丁顿光度的黑洞吸积盘上的尘埃气体

对于中心源是黑洞吸积盘的情况，我们研究了霍伊尔-利特尔顿吸积尘埃气体的情况。通过求解考虑到因灰尘吸收而衰减的辐射力的运动方程，我们揭示了中心物体周围流动的稳定结构。我们发现质量吸积率随着流动光学厚度的增加而增加，即使圆盘光度超过尘埃气体的爱丁顿光度，气体也可以吸积，因为辐射力通过衰减减弱。吸尘。当气体从 Γ′ = 3.0 的圆盘的旋转轴方向流入时，如果 τHL = 3.3，吸积率约为 Hoyle-Lyttleton 吸积率的 $93\%$，对于 τHL = 1.0，吸积率为零，其中Γ′是含尘气体的爱丁顿比，τHL 是霍伊尔-莱特尔顿半径的典型光学厚度。由于盘面方向的辐射通量较小，辐射力往往无法阻止靠近盘面方向的气体吸积。对于 τHL = 3.3 和 Γ′ = 3.4，虽然在 Θ = 0° 的情况下吸积是不可能的，但在 Θ = 90° 的情况下吸积率是 Hoyle-Lyttleton 的 $28\%$，其中 Θ 是气体来自的方向与圆盘的旋转轴之间的角度。我们还获得了相对较高的吸积光度，当圆盘在 BH 上的吸积率与考虑到辐射效应的 Hoyle-Lyttleton 机制的吸积率一致时，我们也获得了相对较高的吸积光度。