We present a method to constrain the temperature of astrophysical black holes through detecting the inspiral phase of binary black hole coalescences. At sufficient separation, inspiraling black holes can be regarded as isolated objects, hence their temperature can still be defined. Due to their intrinsic radiation, inspiraling black holes lose part of their masses during the inspiral phase. As a result, coalescence speeds up, introducing a correction to the orbital phase. We show that this dephasing may allow us to constrain the temperature of inspiraling black holes through gravitational-wave detection. Using the binary black-hole coalescences of the first two observing runs of the Advanced LIGO and Virgo detectors, we constrain the temperature of parental black holes to be less than about $ 10^9 $ K. Such a constraint corresponds to luminosity of about $ 10^{-16} M_{\odot} \rm s^{-1} $ for a black hole of $ 20 M_{\odot} $, which is about 20 orders of magnitude below the peak luminosity of the corresponding gravitational-wave event, indicating no evidence for strong quantum-gravity effects through the detection of the inspiral phase.
Accuracy and precision of gravitational-wave models of inspiraling neutron star -- black hole binaries with spin: comparison with numerical relativity in the low-frequency regime
Searching for Gravitational Waves from the Inspiral of Precessing Binary Systems: Astrophysical Expectations and Detection Efficiency of "Spiky'' Templates
Upper and lower limits on the Crab pulsar's astrophysical parameters set from gravitational wave observations by LIGO: braking index and energy considerations
Probing quantum corrected black hole through astrophysical tests with the orbit of S2 star and quasiperiodic oscillations
Institute of Fundamental and Applied Research, National Research University TIIAME（国立研究大学TIIAME基础与应用研究所）；Institute for Theoretical Physics & Cosmology, Zhejiang University of Technology（浙江工业大学理论物理与宇宙学研究所）；University of Tashkent for Applied Sciences（塔什干应用科学大学）；Center for Theoretical Physics, Khazar University（哈扎尔大学理论物理中心）；School of Physics, Harbin Institute of Technology（哈尔滨工业大学物理学院）；Institute for Advanced Studies, New Uzbekistan University（新乌兹别克斯坦大学高级研究所）；Institute of Theoretical Physics, National University of Uzbekistan（乌兹别克斯坦国立大学理论物理研究所）；United Center for Gravitational Wave Physics (UCGWP), Zhejiang University of Technology（浙江工业大学引力波物理联合中心）
Observational evidence for the formation of trapping horizons in astrophysical black holes
在广义相对论中，黑洞的特征是它们的捕获视界，一种只能向内穿过的单向膜。在天体物理学上，黑洞中的俘获视界的存在可以用反证法（reductio ad absurdum argument）在观测上进行检验，用具有物理表面的无视界结构代替黑洞，并寻找与电磁波和引力波观测不一致的地方。在这种方法中，无水平线物体的半径总是大于但任意接近相同质量的黑洞的视界所在的位置。这些替代方案的半径上限已提供使用电磁观测（在光学/红外波段）的天文源在星系中心，但缺乏下限，留下不受约束的巨大区域的参数空间。我们在这里表明，下限的半径不发展捕获地平线的地平线上的物体，可以放置使用观测吸积系统。这个结果与模型无关，只依赖于由无视界物体周围的时空几何所决定的局部因果关系概念。这些观测范围大大减少了以前允许的参数空间，提高了利用电磁观测建立陷阱视界存在的前景。
Probing Kerr black hole in a uniform Bertotti-Robinson magnetic field through astrophysical quasi-periodic oscillations
Institute for Theoretical Physics and Cosmology, Zhejiang University of Technology（浙江工业大学理论物理与宇宙学研究所）；United Center for Gravitational Wave Physics (UCGWP), Zhejiang University of Technology（浙江工业大学联合引力波物理中心）；Center for Theoretical Physics, Khazar University（哈萨克斯坦大学理论物理中心）；Institute of Fundamental and Applied Research, National Research University TIIAME（国立研究大学塔什干信息技术与应用科学大学基础与应用研究所）；Tashkent University of Applied Sciences（塔什干应用科学大学）；Tashkent State Technical University（塔什干国立技术大学）
