Observations of gravitational waves from massive binary black hole systems at cosmological distances can be used to search for a dependence of the speed of propagation of the waves on wavelength, and thereby to bound the mass of a hypothetical graviton. We study the effects of precessions of the spins of the black holes and of the orbital angular momentum on the process of parameter estimation using matched filtering of gravitational-wave signals vs. theoretical template waveforms. For the proposed space interferometer LISA, we show that precessions, and the accompanying modulations of the gravitational waveforms, are effective in breaking degeneracies among the parameters being estimated, and effectively restore the achievable graviton-mass bounds to levels obtainable from binary inspirals without spin. For spinning, precessing binary black hole systems of equal masses (10^6 solar masses) at 3 Gpc, the bounds on the graviton Compton wavelength achievable are of the order of 5 X 10^{16} km.
Phenomenological Inclusion of Alternative Dispersion Relations to the Teukolsky Equation and its Application to Bounding the Graviton Mass with Gravitational-wave Measurements
Bounding the mass of the graviton using binary pulsar observations
动力学广义相对论对致密双星系统辐射功率的预测与观测到的双星PSR B 1913 +16和PSR B 1534 +12的轨道衰变之间的密切一致性使我们能够以90%的置信度将引力子质量约束为小于7.6 x 10^{-20} eV。这个界限是第一个从动态相对论而不是静态相对论中得到的。由此产生的引力子质量极限与太阳系测量值相差两个数量级，并且可以预期随着进一步的观测而改善。
Rotating black holes in valid vector-tensor theories after GW170817
超越广义相对论的矢量张量理论在引力的紫外线完成的背景下得到了广泛的研究，赋予引力子质量并解释了暗能量现象。在中子星合并事件GW 170817之后，我们在矢量张量理论中构造了旋转黑洞解，该事件对引力波的传播速度提出了严格的限制，使其远离光速.通过对Einstein-Maxwell理论进行一般的保角变换，构造了这样的有效矢量张量理论，并通过对Kerr-Newman解进行同样的保角变换，构造了新的旋转黑洞解.这些理论不属于广义普罗卡理论，但属于扩展类的矢量张量理论，满足退化条件以消除不稳定模式，因此是健康的。我们发现，这样的共形Kerr-Newman解决方案保持的位置的奇异性，事件视界和ergoregion边界从Kerr-Newman，以及多极矩和彼得罗夫型。另一方面，Hamilton-Jacobi方程不再是可分的，这表明在这个解中不存在卡特常数。标准的Newman-Janis算法也不能构造新的解。我们还计算周转频率，最里面的稳定圆轨道的位置，和史瓦西岁差，并将后者应用到最近的重力测量放置从克尔纽曼的Sgr A $^*$的偏差的界限。
