Among the expected sources of gravitational waves for the LaserInterferometer Space Antenna (LISA) is the capture of solar-mass compact starsby massive black holes residing in galactic centers. We construct a simplemodel for such a capture, in which the compact star moves freely on a circularorbit in the equatorial plane of the massive black hole. We consider thegravitational waves emitted during the late stages of orbital evolution,shortly before the orbiting mass reaches the innermost stable circular orbit.We construct a simple model for the gravitational-wave signal, in which thephasing of the waves plays the dominant role. The signal's behavior depends ona number of parameters, including $\mu$, the mass of the orbiting star, $M$,the mass of the central black hole, and $J$, the black hole's angular momentum.We calculate, using our simplified model, and in the limit of largesignal-to-noise ratio, the accuracy with which these quantities can beestimated during a gravitational-wave measurement. Our simplified model alsosuggests a method for experimentally testing the strong-field predictions ofgeneral relativity.
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机译:LaserInterferometer空间天线(LISA)的引力波的预期来源之一是通过位于银河系中心的大量黑洞捕获太阳质量的紧凑恒星。我们为这种捕获构建了一个简单模型,其中紧凑型恒星在大质量黑洞的赤道平面内的圆形轨道上自由移动。我们考虑了在轨道演化后期,即在轨道质量到达最内层稳定圆形轨道之前不久发出的引力波。我们为引力波信号构建了一个简单的模型,其中,波的相位起着主导作用。信号的行为取决于许多参数,包括$ \ mu $,运行中的恒星的质量,$ M $,中心黑洞的质量以及$ J $,黑洞的角动量。简化模型,并且在大信噪比的限制下,可以在引力波测量期间估算这些量的精度。我们的简化模型还建议了一种通过实验测试广义相对论强场预测的方法。
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