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

我们开发了一个数值轴来计算Teukolsky方程的齐次解，Teukolsky方程是黑洞摄动法的基本方程。该代码比以前存在的代码更准确，更高效。通过这个轴，我们计算了一颗恒星围绕克尔黑洞的一般束缚轨道所产生的引力波。我们还计算了由于引力波的线性动量的发射而产生的反冲效应。研究了一种有效的自旋致密双星引力波数据分析方法。我们研究了用几个象象学参数表示波形的一种分析方法的计算效率和检测效率。利用两个激光干涉引力波探测器研究了引力波探测效率。我们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。我们已经定量地表明，在同一地点具有相同方向的两个探测器的情况下，相干策略比重合策略更优越。我们分析了2000-2004年间TAMA300探测器的数据。我们搜索了质量在1-3个太阳质量之间的致密双星的引力波。我们发现没有信号被发现具有很高的统计学意义。我们还获得了银河事件速率的上限，20/年，这是论文发表时最严格的观测上限。

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.