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

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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.