Feedback from Supercritical Disk Accretion Flows: Two-dimensional Radiation-Hydrodynamic Simulations of Stable and Unstable Disks with Radiatively Driven Outflows
Feedback from Supercritical Disk Accretion Flows: Two-dimensional Radiation-Hydrodynamic Simulations of Stable and Unstable Disks with Radiatively Driven Outflows
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DOI：
10.1086/512118
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发表时间：
2007-03
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影响因子：
--
通讯作者：
K. Ohsuga
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作者：
K. Ohsuga
基于二维辐射流体动力学模拟，研究了具有辐射驱动流出的超临界盘吸积流，适用于各种质量输入速率 Ṁinput，即每单位时间从外部区域提供给盘的质量。粘度采用α规定。对于 Ṁinput ≥ 3 × 102LE/c2，我们采用 α = 0.5，并且 α = 0.1；对于 Ṁinput ≤ 102LE/c2，我们仅采用 α = 0.5，其中 LE 是爱丁顿光度，c 是光速。准稳态盘和辐射驱动流出是在质量输入速率远远超过临界速率（Ṁinput > 3 × 102LE/c2）的情况下形成的。那么，圆盘的光度以及流出的动能输出率都超过了爱丁顿光度。中等超临界圆盘，Ṁinput ~ 10-102LE/c2，表现出极限循环振荡。圆盘的光度在爱丁顿光度上上下波动，并且辐射驱动的流出间歇性地出现。流出的时间平均质量、动量和动能输出速率以及圆盘光度随着质量输入速率的增加而增加，对于 α = 0.5 为 ∝Ṁ-Ṁ，对于 α = 0.1 为 ∝Ṁ-Ṁ。我们的数值模拟表明，如果 Ṁinputc2/LE ~ 几个 10 (α = 0.5) 或 ≳ 几个 (α = 0.1)，Silk & Rees 和 King 提出的黑洞质量与核球速度色散之间相关性的辐射驱动流出模型是成功的。
The supercritical disk accretion flow with radiatively driven outflows is studied based on two-dimensional radiation-hydrodynamic simulations for a wide range of the mass input rate, Ṁinput, which is the mass supplied from the outer region to the disk per unit time. The α-prescription is adopted for the viscosity. We employ α = 0.5, as well as α = 0.1, for Ṁinput ≥ 3 × 102LE/c2 and only α = 0.5 for Ṁinput ≤ 102LE/c2, where LE is the Eddington luminosity and c is the speed of light. The quasi-steady disk and radiatively driven outflows form in the case in which the mass input rate highly exceeds the critical rate, Ṁinput > 3 × 102LE/c2. Then, the disk luminosity, as well as the kinetic energy output rate by the outflow, exceeds the Eddington luminosity. The moderately supercritical disk, Ṁinput ~ 10-102LE/c2, exhibits limit-cycle oscillations. The disk luminosity goes up and down across the Eddington luminosity, and the radiatively driven outflows intermittently appear. The time-averaged mass, momentum, and kinetic energy output rates by the outflow, as well as the disk luminosity, increase with an increase of the mass input rate, ∝Ṁ-Ṁ for α = 0.5 and ∝Ṁ-Ṁ for α = 0.1. Our numerical simulations show that the radiatively driven outflow model for the correlation between black hole mass and bulge velocity dispersion proposed by Silk & Rees and King is successful if Ṁinputc2/LE ~ a few 10 (α = 0.5) or ≳ a few (α = 0.1).