论文标题
嵌入在尘土周环盘中的中间质量黑洞的超级伊德丁顿质量生长
Super-Eddington mass growth of intermediate-mass black holes embedded in dusty circumnuclear disks
论文作者
论文摘要
我们执行了第一个三维辐射流体动力学模拟，该模拟研究了嵌入在大规模自我磨碎，尘土飞扬的核积聚磁盘中的中间质量BHS（IMBHS）的生长。我们探讨了质量积聚效率对气体金属性$ z $的依赖性，并以超级 - 埃德丁顿的质量注入从外部银河系磁盘$ \ dot {m} _ {\ rm in} $中的质量注射率，并且发现只有超过Eddington的速度，就可以在尘埃式的较厚的情况下以超过Eddington的速度来喂入中心的BH。在这种情况下，由于光蒸发而从磁盘上流出了质量流出，因此质量注射率的大量部分（$ \ gtrsim 40 \％$）可以喂养中央BH。条件表示为$ \ dot {m} _ {\ rm in}> 2.2 \ times 10^{ - 1} 〜m_ \ odot〜 {\ rm yr yr}^{ - 1} { - 1}（1+z/10^{ - 2} 〜z_ \ odot） km〜s}^{ - 1}）$，其中$ c _ {\ rm s} $是气体磁盘中的音速。随着数值分辨率的增加，剧烈的磁盘碎片降低了磁盘表面密度和通过形成的团块动力加热，使磁盘厚度更高。结果，光效应质量损失率上升，因此固定金属性的临界注射速率增加。该过程使BHS的超级埃德丁顿增长直到BH质量达到$ M _ {\ rm BH} \ SIM 10^{7-8} 〜M_ \ odot $，具体取决于主机深色halo的属性。在原藻的组装中，在质量差异为3-4 $σ$ at $ z \ sim 15-20 $的质量差异为3-4 $σ$中的种子BHS能够经历其快速生长的短期并转移到Eddington限制的增长阶段之后，后来观察到了超级质量的BHS，在$> 6-7-7 $中观察到了超级质量的BHS。
We perform the first three-dimensional radiation hydrodynamical simulations that investigate the growth of intermediate-mass BHs (IMBHs) embedded in massive self-gravitating, dusty nuclear accretion disks. We explore the dependence of mass accretion efficiency on the gas metallicity $Z$ and mass injection at super-Eddington accretion rates from the outer galactic disk $\dot{M}_{\rm in}$, and find that the central BH can be fed at rates exceeding the Eddington rate only when the dusty disk becomes sufficiently optically thick to ionizing radiation. In this case, mass outflows from the disk owing to photoevaporation is suppressed and thus a large fraction ($\gtrsim 40\%$) of the mass injection rate can feed the central BH. The conditions are expressed as $\dot{M}_{\rm in} > 2.2\times 10^{-1}~M_\odot ~{\rm yr}^{-1} (1+Z/10^{-2}~Z_\odot)^{-1}(c_{\rm s}/10~{\rm km~s}^{-1})$, where $c_{\rm s}$ is the sound speed in the gaseous disk. With increasing numerical resolution, vigorous disk fragmentation reduces the disk surface density and dynamical heating by formed clumps makes the disk thickness higher. As a result, the photoevaorative mass-loss rate rises and thus the critical injection rate increases for fixed metallicity. This process enables super-Eddington growth of BHs until the BH mass reaches $M_{\rm BH} \sim 10^{7-8}~M_\odot$, depending on the properties of the host dark-matter halo and metal-enrichment history. In the assembly of protogalaxies, seed BHs that form in overdense regions with a mass variance of 3-4$σ$ at $z\sim 15-20$ are able to undergo short periods of their rapid growth and transits into the Eddington-limited growth phase afterwards to be supermassive BHs observed at $z>6-7$.
