THE STANDING ACCRETION SHOCK INSTABILITY IN THE DISK AROUND THE KERR BLACK HOLE
THE STANDING ACCRETION SHOCK INSTABILITY IN THE DISK AROUND THE KERR BLACK HOLE
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DOI：
10.1088/0004-637x/696/2/2026
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发表时间：
2009-01
期刊：
影响因子：
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通讯作者：
H. Nagakura;S. Yamada
中科院分区：
文献类型：
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作者：
H. Nagakura;S. Yamada
本文是我们以前关于Schwarzschild黑洞吸积和所谓的驻留吸积激波不稳定性的工作的续篇；在这篇文章中，我们研究了Kerr黑洞的非轴对称微扰。通过二维广义相对论流体力学模拟和线性分析，详细分析了激波演化的线性和非线性阶段。由于具有驻波的定常轴对称吸积流的结构对内部跨声速流动非常敏感，其马赫数等对稳定性有重要影响的性质对克尔参数有很大的影响。尽管不稳定性的基本特征与前人对Schwarzschild黑洞的结果没有什么不同，但Kerr黑洞特有的标架拖曳效应也是明显的。有趣的是，基本不稳定模的振荡周期只与激波半径有关，而与注入参数无关。
This paper is a sequel to our previous work for accretion onto a Schwarzschild black hole and the so-called standing accretion shock instability; in this paper, we investigate nonaxisymmetric perturbations for a Kerr black hole. The linear and nonlinear phases for the shock evolution are analyzed in detail by both two-dimensional general relativistic hydrodynamical simulations and linear analysis. Since the structure of steady axisymmetric accretion flows with a standing shock wave is very sensitive to the inner transonic flow, their properties such as Mach numbers, which are important for the stability, depend on the Kerr parameter very much. Although the essential features of the instability do not differ from the previous results for the Schwarzschild black hole, the frame-dragging effects specific to the Kerr black hole are also evident. Interestingly, the oscillation periods of the fundamental unstable modes are dependent only on the shock radius irrespective of the injection parameters.