论文标题
黑洞光谱：测试具有重力波观测的黑洞性质的前景
Black hole spectroscopy: prospects for testing the nature of black holes with gravitational wave observations
论文作者
论文摘要
引力波提供了有关时空性质和黑洞存在的直接信息。二进制黑洞合并的残留物以准模式的形式排放引力波，其光谱被称为黑洞的“指纹”，因为它仅取决于残留物的性质。准模式可用于测试天体物理黑洞与Kerr几何形状匹配的程度。每个模式都通过三个索引进行参数化：谐波数量$（\ ell，m）$和吹式索引$ n $，它们标记了基本模式（$ n = 0 $）和泛音（$ n = 1,2,3，\ ldots $）。黑洞光谱法是使用多种准模式检测进行测试无发性定理的建议。在这项工作中，我们研究了执行黑洞光谱法的前景。 $（2,2,0）$是主导模式，我们分析了数值相对性模拟中最相关的亚辅助模式的贡献。我们表明，泛音模式$（2,2,1）$的幅度更高或可与最相关的较高谐波模式的振幅相当。对于当前和将来的引力波检测器，我们计算黑洞光谱范围，这是事件的最大距离，直到可以检测到两个或多个或多个准模式。对于低质量比二进制文件，次级和第三级模式分别为$（2,2,1）$和$（3,3,0）$，对于大质量比例，$（3,3,0）$和$（4,4,0）$是最相关的属于检测的$（3,3,0）$。我们的工作表明，通过未来重力波检测器检测亚辅助模式的前景有希望的前景。 Ligo的事件率要小得多，但并非如此。
Gravitational waves provide direct information about the nature of spacetime and the existence of black holes. The remnant of a binary black hole merger emits gravitational waves in the form of quasinormal modes, whose spectrum is known as the "fingerprints" of a black hole, as it depends only on the properties of the remnant. The quasinormal modes can be used to test how closely an astrophysical black hole matches the Kerr geometry. Each mode is parameterized by three indices: the harmonic numbers $(\ell, m)$ and the overtone index $n$, that labels the fundamental mode ($n = 0$) and the overtones ($n = 1,2,3,\ldots$). Black hole spectroscopy is the proposal to use the detection of multiple quasinormal modes to test the no-hair theorem. In this work, we investigate the prospects for performing black hole spectroscopy. The $(2,2,0)$ is the dominant mode, and we analyze the contribution of the most relevant subdominant modes in numerical relativity simulations. We show that the overtone mode $(2,2,1)$ has an amplitude higher or comparable to the amplitude of the most relevant higher harmonic modes. For current and future gravitational wave detectors, we compute the black hole spectroscopy horizon, which is the maximum distance of an event up to which two or more quasinormal modes can be detected. For low mass ratio binaries, the secondary and tertiary modes are the $(2,2,1)$ and $(3,3,0)$, respectively, and, for the large mass ratio case, the $(3,3,0)$ and $(4,4,0)$ are the most relevant subdominant modes for detection. Our work indicates promising prospects for the detection of subdominant modes with future gravitational wave detectors. The event rate for LIGO is much smaller, but not prohibitively so.
