吸积环流体动力阻力对极端质量比吸气的影响
The influence of the hydrodynamic drag from an accretion torus on extreme mass-ratio inspirals
摘要：
研究了含有旋转黑洞和具有恒定比角动量的非自引力环面的时空中的极端质量比旋光。我们已经发现，环对卫星施加的流体动力学阻力的影响是远远小于相应的一个由于辐射反应，如那些一般预期在AGN和距离SMBH，可以探测与LISA的系统。然而，由于这些系统的参数的不确定性，存在的配置中的流体动力阻力的效果可以媲美的辐射反应的一个阶段的inspiral这是可检测的LISA。例如，对于被质量相当且半径为10^3-10^4引力半径的共转环面包围的10^6 M_sun SMBH，或者被半径为10^5引力半径的共转10^4 M_sun环面包围的10^5 M_sun SMBH，情况就是如此。如果这些条件在天体物理系统中得到满足，EMRI-引力波就可以提供环存在的特征信号。事实上，虽然辐射反应总是增加轨道相对于赤道平面的倾斜度，但来自与SMBH共转的环面的流体动力阻力总是减小它。然而，即使在最初主导辐射反应时，流体动力阻力的影响也会随着卫星进入SMBH的非常强的场区域（即，p <~ 5M）。虽然我们的结果已经获得了一个特定的类的环面，我们认为，他们将是定性有效的，也为更一般的分布的特定角动量。
英文摘要：
We have studied extreme mass-ratio inspirals (EMRIs) in spacetimes containing a rotating black hole and a non self-gravitating torus with constant specific angular momentum. We have found that the effect of the hydrodynamic drag exerted by the torus on the satellite is much smaller than the corresponding one due to radiation reaction, for systems such as those generically expected in AGNs and at distances from the SMBH which can be probed with LISA. However, given the uncertainty on the parameters of these systems, there exist configurations in which the effect of the hydrodynamic drag can be comparable to the radiation-reaction one in phases of the inspiral which are detectable by LISA. This is the case, for instance, for a 10^6 M_sun SMBH surrounded by a corotating torus of comparable mass and with radius of 10^3-10^4 gravitational radii, or for a 10^5 M_sun SMBH surrounded by a corotating 10^4 M_sun torus with radius of 10^5 gravitational radii. Should these conditions be met in astrophysical systems, EMRI-gravitational waves could provide a characteristic signature of the presence of the torus. In fact, while radiation reaction always increases the inclination of the orbit with respect to the equatorial plane, the hydrodynamic drag from a torus corotating with the SMBH always decreases it. However, even when initially dominating over radiation reaction, the influence of the hydrodynamic drag decays very rapidly as the satellite moves into the very strong-field region of the SMBH (i.e., p <~ 5M). Although our results have been obtained for a specific class of tori, we argue that they will be qualitatively valid also for more generic distributions of the specific angular momentum.
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