Precisely computing bound orbits of spinning bodies around black holes. II. Generic orbits
Precisely computing bound orbits of spinning bodies around black holes. II. Generic orbits
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DOI：
10.1103/physrevd.105.124041
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发表时间：
2022-01
影响因子：
5
通讯作者：
L. Drummond;S. Hughes
中科院分区：
文献类型：
--
作者：
L. Drummond;S. Hughes
在这篇文章中，我们继续研究自转试验体绕克尔黑洞的运动。非自转的测试体遵循它们运动的时空的测地线。一个测试物体的自旋与该时空的曲率相耦合，引入一种“自旋-曲率力”，将物体的世界线推离测地线轨道。自旋曲率力是后测地线效应的一个重要例子，必须仔细建模，以便准确地描述绕黑洞运行的物体的运动。这项工作的一个动机是理解如何在恒星质量物体的气旋产生的引力波模型中包含这种效应到大质量黑洞中。在这篇论文的前身中，我们描述了一种用频域描述来计算黑洞周围自旋物体的束缚轨道的技术，这种描述可以非常精确地求解。本文概述了我们的方法，并给出了偏心和近赤道轨道(即轨道的运动不超过数学上的{O}(S)$离开赤道平面)的结果。在本文中，我们将这个公式应用到完全一般的情况--轨道是倾斜的和偏心的，小天体的自转是任意定向的。我们计算了这些轨道所遵循的轨迹，并计算了小天体的自旋如何影响重要的量，如可观测的轨道频率$\omga_r$、$\omga_\theta$和$\omega_\Phi$。
In this paper, we continue our study of the motion of spinning test bodies orbiting Kerr black holes. Non-spinning test bodies follow geodesics of the spacetime in which they move. A test body's spin couples to the curvature of that spacetime, introducing a"spin-curvature force"which pushes the body's worldline away from a geodesic trajectory. The spin-curvature force is an important example of a post-geodesic effect which must be modeled carefully in order to accurately characterize the motion of bodies orbiting black holes. One motivation for this work is to understand how to include such effects in models of gravitational waves produced from the inspiral of stellar mass bodies into massive black holes. In this paper's predecessor, we describe a technique for computing bound orbits of spinning bodies around black holes with a frequency-domain description which can be solved very precisely. In that paper, we present an overview of our methods, as well as present results for orbits which are eccentric and nearly equatorial (i.e., the orbit's motion is no more than $\mathcal{O}(S)$ out of the equatorial plane). In this paper, we apply this formulation to the fully generic case -- orbits which are inclined and eccentric, with the small body's spin arbitrarily oriented. We compute the trajectories which such orbits follow, and compute how the small body's spin affects important quantities such as the observable orbital frequencies $\Omega_r$, $\Omega_\theta$ and $\Omega_\phi$.