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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Systematic two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model
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Systematic two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model

机译：超爱丁顿增生流动和流出的系统二维辐射-流体动力学模拟：与薄盘模型比较

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To what extent can the one-dimensional slim disk model reproduce the multi-dimensional results of global radiation-hydrodynamic simulations of super-Eddington accretion? With this question in mind, we perform a systematic simulation study of accretion flow onto a non-spinning black hole for a variety of black hole masses of (10–107)?M⊙ and mass accretion rates of (1.4 × 102–5.6 × 103)?LEdd/c2 (with LEdd and c being the Eddington luminosity and the speed of light). In order to adequately resolve large-scale outflow structure, we extensively expand a simulation box to cover the space of 3000?rS (with rS being the Schwarzschild radius), larger than those in most previous studies, so that we can put relatively large angular momentum on the gas injected from the outer simulation boundary. The adopted Keplerian radius, at which the centrifugal force balances the gravitational force, is rK = 300?rS. The injected mass first falls and is accumulated at around this radius and then slowly accretes toward the central black hole via viscosity. We simulate such accretion processes, taking inverse and bulk Compton scattering into account. The simulated accretion flow is in a quasi-steady state inside rqss ～ 200?rS. Within this radius the flow properties are, on the whole, in good agreement with those described by the slim disk model except that the radial density profile of the underlying disk is much flatter, ρ?∝?r?0.73 (cf. ρ?∝?r?3/2 in the slim disk model), due probably to efficient convection. We find very weak outflow from inside r ～ 200?rS, unlike the previous studies.
机译：一维薄盘模型可以在多大程度上再现超级爱丁顿积聚的整体辐射-流体动力学模拟的多维结果？考虑到这个问题，我们对各种（10–107）？M⊙的黑洞质量和（1.4×102–5.6× 103）？LEdd / c2（其中LEdd和c为爱丁顿光度和光速）。为了充分解决大规模的流出结构，我们广泛扩展了一个模拟框，以覆盖3000？rS的空间（rS是Schwarzschild半径），该空间比以前的大多数研究都大，因此我们可以放置相对较大的角度从外部模拟边界注入的气体上的动量。离心力与重力平衡时所采用的开普勒半径为rK = 300？rS。注入的质量首先下降，并在此半径附近聚集，然后通过粘度缓慢向中心黑洞积聚。我们模拟了这种吸积过程，并考虑了康普顿逆散射和体散射。模拟的吸积流在rqss〜200？rS内处于准稳态。在这个半径范围内，流动特性总体上与细长圆盘模型所描述的一致，除了下层圆盘的径向密度分布曲线更平整，ρ？？？r？0.73（参见ρ？？在薄型磁盘模型中为？r？3/2），可能是由于有效的对流。与以前的研究不同，我们发现从r〜200？rS内部流出非常弱。

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