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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：从超临界吸积流到黑洞的块状流出的三维结构

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We perform global three-dimensional (3D) radiation-hydrodynamic (RHD) simulations of outflow from supercritical accretion flow around a 10?M⊙ 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 ～102LE/c2 in the underlying 2D simulation data, and the outflow rate is ～10?LE/c2 (with LE 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 (rS) 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 ～103?rS from the center. The typical clump size is ～30?rS or less in the radial direction, and is more elongated in the angular directions,?～?hundreds of rS at most. The sheet separation ranges from 50 to 150?rS. 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⊙, in rough agreement with the observations of some ultra-luminous X-ray sources.
机译：我们执行围绕10？M⊙黑洞的超临界积积流流出的全局三维（3D）辐射流体动力学（RHD）模拟。我们仅从近似稳态的轴对称2D模拟数据开始，但在方位角方向上以正弦形式添加较小的扰动来求解流出部分。在基础的2D模拟数据中，黑洞上的质量吸积率约为102LE / c2，流出率约为10µLE / c2（LE和c分别是爱丁顿光度和光速）。我们首先确认出现了块状流出，这是通过二维RHD模拟发现的，位于离中心黑洞数百个Schwarzschild半径（rS）的光球上方。作为突出的3D特征，我们发现团块的形状是撕裂的板状，而不是切割的绳子，并且团块围绕中心黑洞旋转，并且距中心约103？rS，处于次开普勒速度。 。典型的团块尺寸在径向方向上约为〜30？rS或更小，而在角度方向上则更为拉长，最大为数百rS。纸页分离范围为50至150？rS。当团块越过遥远的观察者的视线时，我们期望随机的时间变化。对于质量为10至几十M⊙的黑洞，变化时间尺度估计为几秒钟，这与某些超发光X射线源的观测结果大致吻合。

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