标题： 利用引力波观测双致密星系合并限制引力子质量 显示英文标题

标题： Bounding the mass of the graviton using gravitional-wave observations of inspiralling compact binaries

摘要： 如果引力是由一种具有质量的场传播的，那么引力波（引力子）的速度将依赖于它们的频率，而有效的牛顿势将具有反常核力的形式。 对于正在螺旋靠近的致密双星系统，早期螺旋阶段低频发射的引力波会比后期高频发射的引力波稍微慢一些传播，这会修改所观测到的螺旋靠近引力波信号的相位演化，类似于由四极矩相位的后牛顿修正引起的效应。 波形的匹配滤波可以限制这种与频率相关的传播速度变化，并由此限制引力子的质量。 这一限制取决于源的质量以及探测器的噪声特性，但与源的距离无关，除非存在弱的宇宙学红移效应。 对于使用LIGO/VIRGO类型的地面干涉仪观测恒星质量致密天体螺旋靠近的情况，引力子康普顿波长的限制约为$6 \times 10^{12}$公里，大约是牛顿引力的反常核力太阳系测试结果的两倍。 对于使用提议中的激光干涉空间天线（LISA）在宇宙距离上观测超大质量黑洞双星螺旋靠近的情况，这一限制可以达到$6 \times 10^{16}$公里。 这比基于星团动力学的模型依赖性限制弱三个数量级。 显示英文摘要

摘要： If gravitation is propagated by a massive field, then the velocity of gravitational waves (gravitons) will depend upon their frequency and the effective Newtonian potential will have a Yukawa form. In the case of inspiralling compact binaries, gravitational waves emitted at low frequency early in the inspiral will travel slightly slower than those emitted at high frequency later, modifying the phase evolution of the observed inspiral gravitational waveform, similar to that caused by post-Newtonian corrections to quadrupole phasing. Matched filtering of the waveforms can bound such frequency-dependent variations in propagation speed, and thereby bound the graviton mass. The bound depends on the mass of the source and on noise characteristics of the detector, but is independent of the distance to the source, except for weak cosmological redshift effects. For observations of stellar-mass compact inspiral using ground-based interferometers of the LIGO/VIRGO type, the bound on the graviton Compton wavelength is of the order of $6 \times 10^{12}$ km, about double that from solar-system tests of Yukawa modifications of Newtonian gravity. For observations of super-massive black hole binary inspiral at cosmological distances using the proposed laser interferometer space antenna (LISA), the bound can be as large as $6 \times 10^{16}$ km. This is three orders of magnitude weaker than model-dependent bounds from galactic cluster dynamics.