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Research of the gravitational radiation by means of the black hole perturbation method and the post-Newtonian approximation

利用黑洞微扰法和后牛顿近似研究引力辐射

基本信息

批准号：
16540251
负责人：
TAGOSHI Hideyuki
金额：
$ 2.48万
依托单位：
Osaka University
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (C)
财政年份：
2004
资助国家：
日本
起止时间：
2004 至 2007
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16540251/
关键词：
general relativity gravitational radiation black hole gravitational wave detector neutron star astrophysics

项目摘要

We developed a numerical axle to compute the homogeneous solutions of the Teukolsky equation, which is the basic equation of the black hole perturbation method. The code is more accurate and more efficient than the code existed before. With this axle, we computed the gravitational waves from a star orbiting a generic bound orbit around a Kerr black hole. We also computed the recoil effect due to the emission of the linear momentum of gravitational waves.We investigated an efficient data analysis methods of gravitational waves from inspiraling spinning compact binaries. We studies the computational efficiency and the detection efficiency of an analysis method in which the waveforms are expressed in terms of a few phenomenological parameters.We investigated the detection efficiency of the gravitational waves from inspiraling compact binaries using two laser interferometric gravitational wave detectors. We compared the conventional coincident detection strategy and the coherent detection strategy. The coherent strategy is a method based on the maximum likelihood detection strategy. We have shown quantitatively, in the case of two detectors in the same site with the same orientation, that the coherent strategy is more superior than the coincident strategy.We have analyzed the data from TAMA300 detectors during the years, 2000-2004. We searched for the gravitational waves from inspiraling compact star binaries with mass between 1-3 solar mass. We found that the no signal were found with high statistical significance. We also obtained the upper limit on the Galactic event rate, 20/year, which was the most stringent observational upper limit at the time when the paper was published.

我们开发了一个数值轴来计算Teukolsky方程的齐次解，这是黑洞微扰法的基本方程。该代码比以前的代码更准确，更有效。利用这个轴，我们计算了一颗绕克尔黑洞一般束缚轨道运行的星星的引力波。我们还计算了引力波线动量发射引起的反冲效应，研究了一种有效的旋进致密双星引力波数据分析方法。研究了波形用唯象参数表示的分析方法的计算效率和探测效率，并利用两台激光干涉引力波探测器研究了引力波在吸入型致密双星中的探测效率。比较了传统的重合检测策略和相干检测策略。相干策略是一种基于最大似然检测策略的方法。我们定量地表明，在同一地点的两个探测器具有相同的方向的情况下，相干的策略是更上级比重合的策略。我们分析了数据从TAMA 300探测器在几年，2000-2004。我们寻找引力波从吸入紧凑的星星双星质量之间的1-3太阳质量。我们发现，无信号被发现具有高度的统计学意义。我们还获得了银河系事件发生率的上限，20/年，这是论文发表时最严格的观测上限。