Evolution of growing black holes in axisymmetric galaxy cores
Evolution of growing black holes in axisymmetric galaxy cores
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DOI：
10.1111/j.1365-2966.2011.19670.x
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发表时间：
2011-08
影响因子：
4.8
通讯作者：
J. Fiestas;O. Porth;P. Berczik;R. Spurzem
中科院分区：
文献类型：
--
作者：
J. Fiestas;O. Porth;P. Berczik;R. Spurzem
本文介绍了具有生长黑洞的轴对称碰撞星系核（如M32、M33、NGC205、银河系）的N体实现。接近瓦解球的恒星被瓦解并吸积到黑洞中。我们测量的黑洞和破坏率的影响区域的弛豫时间尺度。我们表明，长期的引力不稳定性占主导地位的初始核心动力学，而黑洞是小的，由于恒星的消费和增长。后来，黑洞势主导核心，可以应用损失锥理论。我们的模拟结果表明，星系的中心旋转是不可忽略的松弛系统，并比较和讨论我们的结果与球对称系统的标准理论。
N-body realizations of axisymmetric collisional galaxy cores (e.g. M32, M33, NGC 205, Milky Way) with embedded growing black holes are presented. Stars which approach the disruption sphere are disrupted and accreted to the black hole. We measure the zone of influence of the black hole and disruption rates in relaxation time-scales. We show that secular gravitational instabilities dominate the initial core dynamics, while the black hole is small and growing due to the consumption of stars. Later, the black hole potential dominates the core, and the loss cone theory can be applied. Our simulations show that central rotation in galaxies cannot be neglected for relaxed systems, and compare and discuss our results with the standard theory of spherically symmetric systems.