Gravitational waves from a compact star in a circular, inspiral orbit, in the equatorial plane of a massive, spinning black hole, as observed by LISA
Gravitational waves from a compact star in a circular, inspiral orbit, in the equatorial plane of a massive, spinning black hole, as observed by LISA
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DOI：
10.1103/physrevd.62.124021
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发表时间：
2000-07
影响因子：
5
通讯作者：
L. Finn;K. R. D. O. Physics;AstronomyAstrophysics;T. O. S. University;U. Park;Pa;T. Astrophysics;C. I. O. Technology.;Pasadena;Ca
中科院分区：
文献类型：
--
作者：
L. Finn;K. R. D. O. Physics;AstronomyAstrophysics;T. O. S. University;U. Park;Pa;T. Astrophysics;C. I. O. Technology.;Pasadena;Ca
结果是从高精度计算的轨道演化和发射的引力波的恒星质量的物体螺旋进入一个大质量的黑洞在一个缓慢收缩，圆形，赤道轨道。这些计算的重点是在最内层稳定圆轨道（isco）附近的inspiral-更具体地说，在inspiral的最后一年，在r 0 =1 Gpc时，角速度Ω为0.03 <$Ω/Ωisco 10的轨道。在信噪比大于10的情况下，黑洞的自旋a对M的范围（μ固定时）的影响系数为10，而白矮星双星背景的存在或不存在对M的影响系数为10。与预测的事件发生率进行比较，显示出探测这些波的强烈希望，但如果螺旋状物体是白色矮星或中子星星，则不会超过约1 Gpc。这就要求适度降低丽莎的本底噪声。简要讨论了从观测波中提取信息的前景。
Results are presented from high-precision computations of the orbital evolution and emitted gravitational waves for a stellar-mass object spiraling into a massive black hole in a slowly shrinking, circular, equatorial orbit. The focus of these computations is inspiral near the innermost stable circular orbit (isco)—more particularly, on orbits for which the angular velocity Ω is 0.03≲Ω/Ωisco 10 at r0=1 Gpc during the last year of inspiral. The hole’s spin a has a factor of ∼10 influence on the range of M (at fixed μ) for which S/N>10, and the presence or absence of a white-dwarf–binary background has a factor of ∼3 influence. A comparison with predicted event rates shows strong promise for detecting these waves, but not beyond about 1 Gpc if the inspiraling object is a white dwarf or neutron star. This argues for a modest lowering of LISA’s noise floor. A brief discussion is given of the prospects for extracting information from the observed waves.