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We compute the spectrum and the waveform of gravitational waves generated bythe inspiral of a disk or a spherical like dust body into a Kerr black hole. Weinvestigate the effect of the radius R of the body on gravitational waves andconclude that the radius is inferred from the gravitational wave signalirrespective of (1) the form of the body (a disk or a spherical star) (2) thelocation where the shape of the body is determined, (3) the orbital angularmomentum of the body, and (4) a black hole rotation. We find that when $R$ ismuch larger than the characteristic length of the quasinormal mode frequency,the spectrum has several peaks and the separation of the troughs $\Delta\omega$is proportional to $R^{-1}$. Thus, we may directly determine the radius of astar in a coalescing binary black hole - star system from the observed spectrumof gravitational waves. For example, both trough frequency of neutron stars andwhite dwarfs are within the detectable frequency range of some laserinterferometers and resonant type detectors so that this effect can be observedin the future. We therefore conclude that the spectrum of gravitational wavesmay provide us important signals in gravitational wave astronomy as in opticalastronomy.

Possible direct method to determine the radius of a star from the spectrum of gravitational wave signals. II. Spectra for various cases