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

Motoyuki Saijo*, Takashi Nakamura

*この研究の対応する著者

研究成果: Article査読

10 被引用数 (Scopus)

抄録

We compute the spectrum and the waveform of gravitational waves generated by the inspiral of a disk or a spherical like dust body into a Kerr black hole. We investigate the effect of the radius R of the body on gravitational waves and conclude that the radius is inferred from the gravitational wave signal irrespective of (1) the form of the body (a disk or a spherical star), (2) the location where the shape of the body is determined, (3) the orbital angular momentum of the body, and (4) a black hole rotation. We find that when R is much larger than the characteristic length of the quasinormal mode frequency, the spectrum has several peaks and the separation of the troughs (Formula presented) is proportional to (Formula presented) Thus, we may directly determine the radius of a star in a coalescing binary black hole–star system from the observed spectrum of gravitational waves. For example, both trough frequencies of neutron stars and white dwarfs are within the detectable frequency range of some laser interferometers and resonant type detectors so that this effect can be observed in the future. We therefore conclude that the spectrum of gravitational waves may provide us important signals in gravitational wave astronomy as in optical astronomy.

本文言語English
ページ数1
ジャーナルPhysical Review D - Particles, Fields, Gravitation and Cosmology
63
6
DOI
出版ステータスPublished - 2001 1月 1
外部発表はい

ASJC Scopus subject areas

  • 核物理学および高エネルギー物理学
  • 物理学および天文学(その他)

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