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

Research output: Contribution to journalArticle

10 Citations (Scopus)

Abstract

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.

Original languageEnglish
Number of pages1
JournalPhysical Review D - Particles, Fields, Gravitation and Cosmology
Volume63
Issue number6
DOIs
Publication statusPublished - 2001 Jan 1
Externally publishedYes

Fingerprint

gravitational waves
stars
radii
troughs
astronomy
coalescing
neutron stars
waveforms
interferometers
angular momentum
dust
frequency ranges
orbitals
detectors
lasers

ASJC Scopus subject areas

  • Nuclear and High Energy Physics
  • Physics and Astronomy (miscellaneous)

Cite this

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abstract = "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.",
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AU - Nakamura, Takashi

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N2 - 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.

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