论文标题
在不断扩展的宇宙中，来自紧凑型二进制二进制二进制二进制的灵感的引力波形
Gravitational waveforms from the inspiral of compact binaries in the Brans-Dicke theory in an expanding Universe
论文作者
论文摘要
在修改的重力理论（例如Brans-Dicke理论）中，宇宙的背景演变及其周围的扰动与一般相对性不同。因此，应修改用于研究这些理论中标准警笛的重力波形。波形的修改可以分为两类：波产生效应和波传播效应。迄今为止，用于研究改性重力理论中标准警笛的波形仅包含波传播效应并忽略波产生效应。虽然侧重于波产生效应的波形（例如牛顿后波形）并未结合波传播效应，并且不能直接应用于具有不可忽视的红移的源。在这项工作中，我们在Brans-Dicke理论中为标准警笛构建了一致的波形。波浪产生效果包括标量呼吸极化$ H_B $的排放以及张量极化的校正$ h _+$和$ h_ \ times $;波传播效果是重力波形的光度距离的修饰。使用一致的波形，我们分析了由于波产生效应的无知而分析参数估计偏差。考虑到爱因斯坦望远镜的观察结果，我们发现理论偏差与红移chirp质量的统计误差的比率比源距离的量度大于两个数量级。对于像GW191219这样的黑孔 - 中子恒星二进制系统，红移chirp质量的理论偏置可能比统计误差大几倍。
In modified gravity theories, such as the Brans-Dicke theory, the background evolution of the Universe and the perturbation around it are different from that in general relativity. Therefore, the gravitational waveforms used to study standard sirens in these theories should be modified. The modifications of the waveforms can be classified into two categories: wave generation effects and wave propagation effects. Hitherto, the waveforms used to study standard sirens in the modified gravity theories incorporate only the wave propagation effects and ignore the wave generation effects; while the waveforms focusing on the wave generation effects, such as the post-Newtonian waveforms, do not incorporate the wave propagation effects and cannot be directly applied to the sources with non-negligible redshifts in the study of standard sirens. In this work, we construct the consistent waveforms for standard sirens in the Brans-Dicke theory. The wave generation effects include the emission of the scalar breathing polarization $h_b$ and the corrections to the tensor polarizations $h_+$ and $h_\times$; the wave propagation effect is the modification of the luminosity distance for the gravitational waveforms. Using the consistent waveforms, we analyze the parameter estimation biases due to the ignorance of the wave generation effects. Considering the observations by the Einstein Telescope, we find that the ratio of the theoretical bias to the statistical error of the redshifted chirp mass is two orders of magnitude larger than that of the source distance. For black hole-neutron star binary systems like GW191219, the theoretical bias of the redshifted chirp mass can be several times larger than the statistical error.
