具有驼峰诱导振荡的扩展轨道共振模型
Extended orbital resonance model with hump-induced oscillations
摘要：
在快速旋转的Kerr黑洞中发现了LNRF速度梯度的符号变化，其中Keplerian盘的自旋a > 0.9953，而在边缘稳定的厚盘中自旋a > 0.99979。这样一个“驼峰”LNRF速度配置文件发生在边缘稳定的圆形测地线的上方，可能与吸积盘的振荡。这种“驼峰”引起的振荡的频率可以用“驼峰”轮廓内轨道速度的最大变化率来确定。因此，我们引入一个扩展的轨道共振模型（EXORM）的准周期振荡（QPOs）假设非线性共振现象之间的振荡与轨道周转频率和驼峰频率定义在一个完全广义相对论的方式。的EXORM开发的开普勒光盘和完美流体环面的近似的振荡与周转频率是可以接受的。显然，EXORM可以应用于表现出相对复杂的QPO频率模式的近极端克尔黑洞系统。假设一个开普勒圆盘，它可以表明，在EXORM的框架下，在微类星体GRS 1915+105中观察到的所有QPO都可以解释，而在银河系中心源Sgr A* 中观察到的QPO则是不可能的。
英文摘要：
Change of sign of the LNRF-velocity gradient has been found for accretion discs orbiting rapidly rotating Kerr black holes with spin a > 0.9953 for Keplerian discs and a > 0.99979 for marginally stable thick discs. Such a "humpy" LNRF-velocity profiles occur just above the marginally stable circular geodesic and could be related to oscillations of accretion discs. The frequency of such "hump"-induced oscillations can be identified with the maximal rate of change of the orbital velocity within the "humpy" profile. Therefore, we introduce an extended orbital resonance model (EXORM) of quasiperiodic oscillations (QPOs) assuming non-linear resonant phenomena between oscillations with the orbital epicyclic frequencies and the humpy frequency defined in a fully general relativistic way. The EXORM is developed for both Keplerian discs and perfect-fluid tori where the approximation of oscillations with epicyclic frequencies is acceptable. Clearly, the EXORM could be applied to the near-extreme Kerr black hole systems exhibiting relatively complex QPO frequency patterns. Assuming a Keplerian disc, it can be shown that in the framework of the EXORM, all the QPOs observed in the microquasar GRS 1915+105 could be explained, while it is not possible in the case of QPOs observed in the Galactic Centre source Sgr A*.
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