Gravitational waves from a spinning particle plunging into a Kerr black hole

M. Saijo, K. Maeda

研究成果: Article査読

53 被引用数 (Scopus)

抄録

Using a black hole (BH) perturbation approach, we numerically study gravitational waves from a spinning particle of mass (Formula presented) and spin (Formula presented) on the equatorial plane plunging into a Kerr BH of mass (Formula presented) and spin (Formula presented) When we take into account the particle spin (Formula presented) (a) the motion of the particle changes due to the coupling effects between (Formula presented) and the orbital angular momentum (Formula presented) and between (Formula presented) and (Formula presented) and also (b) the energy momentum tensor of the linearized Einstein equations changes. We calculate the total radiated energy, linear momentum, angular momentum, the energy spectrum, and waveform of gravitational waves, and we find the following features. (1) There are three spin coupling effects: between (Formula presented) and (Formula presented) between (Formula presented) and (Formula presented) and between (Formula presented) and (Formula presented) when (Formula presented) is considered. Among them, (Formula presented) coupling is the most important effect for the amount of gravitational radiation, and the other two effects are not as remarkable as the first one. However, these effects are still important; for example, the total radiated energy changes by a factor of (Formula presented) for the case of (Formula presented) (Formula presented) if we change (Formula presented) from (Formula presented) to (Formula presented) (2) For the case when one of the three spins (Formula presented) and (Formula presented) is vanishing, the amount of gravitational radiation becomes larger (smaller) if spin axes of the other two are parallel (antiparallel). For the case when three spins are nonvanishing, the amount of gravitational radiation becomes maximum if all the axial directions of (Formula presented) (Formula presented) and (Formula presented) coincide. Thus, our calculations indicate that in a coalescence of two black holes (BHs) whose spins and orbital angular momentum are aligned, gravitational waves are emitted most efficiently.

本文言語English
ジャーナルPhysical Review D - Particles, Fields, Gravitation and Cosmology
58
6
DOI
出版ステータスPublished - 1998

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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