Studies of accretion flows around rotating black holes – II. Standing shocks in the pseudo‐Kerr geometry
Studies of accretion flows around rotating black holes – II. Standing shocks in the pseudo‐Kerr geometry
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DOI：
10.1111/j.1365-2966.2006.10765.x
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发表时间：
2006-09
影响因子：
4.8
通讯作者：
S. Mondal;S. Chakrabarti
中科院分区：
文献类型：
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作者：
S. Mondal;S. Chakrabarti
驻波、传播波或振荡波在致密物体周围的吸积和风中很常见。我们使用伪克尔几何研究所有可能解决方案的拓扑。我们给出了比能量和角动量所跨越的参数空间，并将其与从完整广义相对论获得的参数空间进行比较，表明只要适当修改多变指数，势能也可以在流体动力学中令人满意地发挥作用。然后，我们根据解决方案拓扑的性质划分参数空间。我们专门研究了常设朗肯-于贡尼奥冲击的性质。我们还表明，随着克尔参数的增加，激波位置通常会移近黑洞。将来，这些解决方案可以用作测试紧凑物体周围数值模拟的指南。
Standing, propagating or oscillating shock waves are common in accretion and winds around compact objects. We study the topology of all possible solutions using the pseudo-Kerr geometry. We present the parameter space spanned by the specific energy and angular momentum and compare it with that obtained from the full general relativity to show that the potential can work satisfactorily in fluid dynamics also, provided the polytropic index is suitably modified. We then divide the parameter space depending on the nature of the solution topology. We specifically study the nature of the standing Rankine-Hugoniot shocks. We also show that as the Kerr parameter is increased, the shock location generally moves closer to the black hole. In future, these solutions can be used as guidelines to test numerical simulations around compact objects.