Large-scale outflow structure and radiation properties of super-Eddington flow: Dependence on the accretion rates
Large-scale outflow structure and radiation properties of super-Eddington flow: Dependence on the accretion rates
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超爱丁顿流的大尺度流出结构和辐射特性：对吸积率的依赖
DOI：
10.1093/pasj/psac076
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发表时间：
2022
期刊：
影响因子：
--
通讯作者：
Takaaki
中科院分区：
文献类型：
--
作者：
Yoshioka;Shogo ; Mineshige;Shin ; Ohsuga;Ken ; Kawashima;Tomohisa ; Kitaki;Takaaki
为了准确地评估超爱丁顿吸积体对环境的影响，必须保证足够大的模拟箱和较长的计算时间，以尽可能避免数值设置中的任何伪影。本文在大型模拟箱中对10 M ~ 2黑洞进行了轴对称二维辐射流体动力学模拟，研究了不同黑洞吸积率下超爱丁顿吸积流的大尺度外流结构和辐射性质（其中LEd为爱丁顿光度，c为光速）.流入物质的开普勒半径（离心力与重力平衡时）固定为2430史瓦西半径。我们发现，机械发光度的增长比辐射发光度的增长更快。特别是当从近正面方向看时，各向同性机械光度与成比例地增长，而总机械光度与成比例地增长。前者的原因是，越高，盘表面变得越垂直膨胀，这使得辐射场更多地局限在旋转轴周围的区域，从而强烈地加速流出的气体。根据流出的气体是否能到达模拟箱的外边界，流出分为纯流出和失败流出。的减少，失败流出的分数减少。我们分析物理量沿沿着每个流出轨迹，发现伯努利参数（Be）是不是一个很好的指标，以区分纯和失败的流出，因为它从来没有恒定的，因为辐射压力的连续加速。即使在发射点Be < 0，也会出现纯外流。
In order to evaluate the impacts made by super-Eddington accretors on their environments precisely, it is essential to guarantee a large enough simulation box and long computational time to avoid any artefacts from numerical settings as much as possible. In this paper, we carry out axisymmetric two-dimensional radiation hydrodynamic simulations around a 10M⊙black hole in large simulation boxes and study the large-scale outflow structure and radiation properties of super-Eddington accretion flow for a variety of black hole accretion rates,(withLEddbeing the Eddington luminosity andcbeing the speed of light). The Keplerian radius of the inflow material, at which centrifugal force balances with gravitational force, is fixed to 2430 Schwarzschild radii. We find that the mechanical luminosity grows more rapidly than the radiation luminosity with an increase of. When seen from a nearly face-on direction, especially, the isotropic mechanical luminosity grows in proportion to, while the total mechanical luminosity is proportional to. The reason for the former is that the higheris, the more vertically inflated the disk surface becomes, which makes radiation fields more confined in the region around the rotation axis, thereby strongly accelerating outflowing gas. The outflow is classified into pure outflow and failed outflow, depending on whether the outflowing gas can reach the outer boundary of the simulation box or not. The fraction of the failed outflow decreases with a decrease of. We analyze physical quantities along each outflow trajectory, finding that the Bernoulli parameter (Be) is not a good indicator to discriminate between pure and failed outflows, since it is never constant because of continuous acceleration by radiation-pressure force. Pure outflow can arise, even ifBe< 0 at the launching point.