TY - JOUR

T1 - Gravitational waves from a spinning particle plunging into a Kerr black hole

AU - Saijo, M.

AU - Maeda, K.

PY - 1998/1/1

Y1 - 1998/1/1

N2 - 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.

AB - 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.

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U2 - 10.1103/PhysRevD.58.064005

DO - 10.1103/PhysRevD.58.064005

M3 - Article

AN - SCOPUS:0542418899

VL - 58

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

SN - 1550-7998

IS - 6

ER -