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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Three-dimensional structure of clumpy outflow from supercritical accretion flow onto black holes
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Three-dimensional structure of clumpy outflow from supercritical accretion flow onto black holes

机译：超临界空转流入黑洞的三维结构

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We perform global three-dimensional (3D) radiation-hydrodynamic (RHD) simulations of outflow from supercritical accretion flow around a 10 M-circle dot black hole. We only solve the outflow part, starting from the axisymmetric 2D simulation data in a nearly steady state but with small perturbations in a sinusoidal form being added in the azimuthal direction. The mass accretion rate onto the black hole is similar to 10(2) L-E/c(2) in the underlying 2D simulation data, and the outflow rate is similar to 10 L-E/c(2) (with L-E and c being the Eddington luminosity and speed of light, respectively). We first confirm the emergence of clumpy outflow, which was discovered by the 2D RHD simulations, above the photosphere located at a few hundreds of Schwarzschild radii (r(S)) from the central black hole. As prominent 3D features we find that the clumps have the shape of a torn sheet, rather than a cut string, and that they are rotating around the central black hole with a sub-Keplerian velocity at a distance of similar to 10(3) r(S) from the center. The typical clump size is similar to 30 r(S) or less in the radial direction, and is more elongated in the angular directions, similar to hundreds of r(S) at most. The sheet separation ranges from 50 to 150 r(S). We expect stochastic time variations when clumps pass across the line of the sight of a distant observer. Variation timescales are estimated to be several seconds for a black hole with mass of ten to several tens of M-circle dot, in rough agreement with the observations of some ultra-luminous X-ray sources.
机译：我们对一个10米圆点黑洞周围的超临界吸积流的流出进行了全局三维（3D）辐射流体力学（RHD）模拟。我们只解决流出部分，从轴对称二维模拟数据开始，在几乎稳定的状态下，但在方位方向添加正弦形式的小扰动。黑洞上的质量吸积率类似于基础2D模拟数据中的10（2）L-E/c（2），而流出率类似于10 L-E/c（2）（L-E和c分别是Eddington光度和光速）。我们首先确认了在距离中心黑洞几百个施瓦西半径（r（S））的光球上方出现的块状流出，这是由2D RHD模拟发现的。作为突出的3D特征，我们发现这些团块的形状是撕裂的薄片，而不是切割的弦，它们以亚开普勒速度围绕中心黑洞旋转，距离中心的距离类似于10（3）r（S）。典型的束大小在径向上类似于30 r（S）或更小，在角度方向上更细长，最多类似于数百r（S）。板材间距范围为50至150 r（S）。当束流穿过远处观察者的视线时，我们预计会出现随机的时间变化。对于质量为10到几十个M圆点的黑洞，变化时间尺度估计为几秒钟，这与一些超发光X射线源的观测结果大致一致。

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