论文标题
黑洞X射线二进制的准周期振荡的几何起源
A geometric origin for quasi-periodic oscillations in black hole X-ray binaries
论文作者
论文摘要
我们将相对论的预性模型扩展到包括非试点和偏心轨迹，并将其应用于黑洞X射线二进制文件（BHXRBS）中的准周期振荡（QPO）（QPO）轨迹，在克尔黑洞附近。我们研究了使用两个或三个同时QPO的案例，并提取参数\ {$ e $，$ r_p $，$ a $，$ q $ \}，其中$ r_p $是轨道的periastron距离，而$ a $是黑洞的旋转。我们发现，对于观察到的qPO频率范围的$ e \ lyssim 0.5 $和$ e \ sim 2-20 $，$ e \ e \ sim 2-20 $的轨道应具有$ e \ e \ lyssim 0.5 $和$ r_p \ sim 2-20 $，其中$ a \ in [0,1] $，而球形轨迹\ e = 0 $ e = 0 $ q \ q \ q \ q \ q \ n $ \ sim 3-20 $。我们发现M82 X-1和GROJ 1655-40的非试价偏心解决方案。我们看到这些轨迹在一起时跨越了圆环区域并产生强烈的QPO信号。对于两个同时QPO病例，我们找到了XTEJ 1550-564、4U 1630-47和GRS 1915+105的赤道偏心轨道溶液，以及用于BHXRBS M82 X-1和XTEJ 1550-564的球形轨道溶液。我们还表明，偏心轨道溶液符合BHXRB GROJ 1655-40中观察到的psaltis-belloni-klis相关性。我们对相对论磁盘边缘中流体流动的分析表明，不稳定性导致QPO源于圆环区域。我们还为球形和赤道偏心轨道的轨迹和频率提供了一些有用的公式。
We expand the relativistic precession model to include nonequatorial and eccentric trajectories and apply it to quasi-periodic oscillations (QPOs) in black hole X-ray binaries (BHXRBs) and associate their frequencies with the fundamental frequencies of the general case of nonequatorial (with Carter's constant, $Q\neq 0$) and eccentric ($e\neq 0$) particle trajectories, around a Kerr black hole. We study cases with either two or three simultaneous QPOs and extract the parameters \{$e$, $r_p$, $a$, $Q$\}, where $r_p$ is the periastron distance of the orbit, and $a$ is the spin of the black hole. We find that the orbits with $\left[Q=0-4\right]$ should have $e\lesssim 0.5$ and $r_p \sim 2-20$ for the observed range of QPO frequencies, where $a \in [0,1]$, and that the spherical trajectories \{$e=0$, $Q \neq0$\} with $Q=2-4$ should have $r_s \sim 3-20$. We find nonequatorial eccentric solutions for both M82 X-1 and GROJ 1655-40. We see that these trajectories, when taken together, span a torus region and give rise to a strong QPO signal. For two simultaneous QPO cases, we found equatorial eccentric orbit solutions for XTEJ 1550-564, 4U 1630-47, and GRS 1915+105, and spherical orbit solutions for BHXRBs M82 X-1 and XTEJ 1550-564. We also show that the eccentric orbit solution fits the Psaltis-Belloni-Klis correlation observed in BHXRB GROJ 1655-40. Our analysis of the fluid flow in the relativistic disk edge suggests that instabilities cause QPOs to originate in the torus region. We also present some useful formulae for trajectories and frequencies of spherical and equatorial eccentric orbits.
