论文标题
用于旋转二进制黑洞的多极引力波形及其对源表征的影响
Multipolar gravitational waveforms for spinning binary black holes and their impact on source characterization
论文作者
论文摘要
在过去的五年中，引力波天文学已从纯粹的理论领域变成了蓬勃发展的实验科学。已经检测到许多由恒星质量的二进制黑洞和二进制中子星排出的引力波信号，并且将来会预计会有更多。从这些系统中观察引力波信号及其来源的表征，很大程度上取决于发射的引力波形的精确模型。在本文中，我提出了一个更新的波形模型，用于在有效的体式形式中旋转二进制黑洞。这项工作中介绍的波形模型的新颖性是通过旋转二进制黑洞发出的波形中包含了超级术语。我首先在简化的黑洞中构建模型，其旋转与二进制的轨道角动量对齐，然后将其扩展到通用旋转方向的情况。发射引力波的二进制系统源特性的测量需要计算$ \ Mathcal {O}（10^7-10^9）$不同的波形。由于前面提到的波形模型可能需要$ \ MATHCAL {O}（1-10）$ S来生成单个波形，因此它们在数据分析研究中很难使用。为了克服这一障碍，我使用降低的订购模型技术来开发更快的版本的黑洞波形模型，其旋转与二进制的轨道角动量对齐。在本文中开发的波形模型已被Ligo和处女座协作使用，用于推断在Ligo和Pirgo探测器的第二和第三观测运行（O2和O3）中检测到的重力波信号的源参数。在这里，我介绍了一项有关信号GW170729和GW190412的源特性的研究，我直接参与了分析。
In the last five years, gravitational-wave astronomy has gone from a purely theoretical field into a thriving experimental science. Many gravitational-wave signals, emitted by stellar-mass binary black holes and binary neutron stars, have been detected, and many more are expected in the future. The observation of the gravitational-wave signals from these systems, and the characterization of their sources, heavily relies on the precise models for the emitted gravitational waveforms. In this thesis, I present an updated version of the waveform models for spinning binary black holes within the effective-one-body formalism. The novelty of the waveform models presented in this work is the inclusion of beyond-quadupolar terms in the waveforms emitted by spinning binary black holes. I first construct the model in the simplified case of black holes with spins aligned with the orbital angular momentum of the binary, then I extend it to the case of generic spin orientations. The measurement of the source properties of a binary system emitting gravitational waves requires to compute $\mathcal{O}(10^7-10^9)$ different waveforms. Since the waveform models mentioned before can require $\mathcal{O}(1-10)$s to generate a single waveform, they can be difficult to use in data-analysis studies. To overcome this obstacle, I use the reduced-order-modeling technique to develop a faster version of the waveform model for black holes with spins aligned to the orbital angular momentum of the binary. The waveform models developed in this thesis have been used by the LIGO and Virgo collaborations for the inference of the source parameters of the gravitational-wave signals detected during the second and third observing runs (O2 and O3) of the LIGO and Virgo detectors. Here, I present a study on the source properties of the signals GW170729 and GW190412, for which I have been directly involved in the analysis.
