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Gravitational waves from a spinning particle scattered by a relativistic star: axial mode case

Gravitational waves from a spinning particle scattered by a relativistic star: axial mode case
Gravitational waves from a spinning particle scattered by a relativistic star: axial mode case
We use a perturbation method to study gravitational waves from a spinning test particle scattered by a relativistic star. The present analysis is restricted to axial modes. By calculating the energy spectrum, the wave forms, and the total energy and angular momentum of gravitational waves, we analyze the dependence of the emitted gravitational waves on particle spin. For a normal neutron star, the energy spectrum has one broad peak whose characteristic frequency corresponds to the angular velocity at the turning point (a periastron). Since the turning point is determined by the orbital parameter, there exists a dependence of the gravitational wave on particle spin. We find that the total energy of l=2 gravitational waves gets larger as the spin increases in the antiparallel direction to the orbital angular momentum. For an ultracompact star, in addition to such an orbital contribution, we find the quasinormal modes excited by a scattered particle, whose excitation rate to gravitational waves depends on the particle spin. We also discuss the ratio of the total angular momentum to the total energy of gravitational waves and explain its spin dependence.
1550-7998
124012-[15pp]
Tominaga, Kazuhiro
334e9997-4cc7-46e9-a4c4-3a8fa7944f5f
Saijo, Motoyuki
f2128aae-e896-4290-a382-d413c868a617
Maeda, Kei-ichi
37d90f1c-3650-42db-8be2-77b1540b6fd8
Tominaga, Kazuhiro
334e9997-4cc7-46e9-a4c4-3a8fa7944f5f
Saijo, Motoyuki
f2128aae-e896-4290-a382-d413c868a617
Maeda, Kei-ichi
37d90f1c-3650-42db-8be2-77b1540b6fd8

Tominaga, Kazuhiro, Saijo, Motoyuki and Maeda, Kei-ichi (2001) Gravitational waves from a spinning particle scattered by a relativistic star: axial mode case. Physical Review D, 63 (12), 124012-[15pp]. (doi:10.1103/PhysRevD.63.124012).

Record type: Article

Abstract

We use a perturbation method to study gravitational waves from a spinning test particle scattered by a relativistic star. The present analysis is restricted to axial modes. By calculating the energy spectrum, the wave forms, and the total energy and angular momentum of gravitational waves, we analyze the dependence of the emitted gravitational waves on particle spin. For a normal neutron star, the energy spectrum has one broad peak whose characteristic frequency corresponds to the angular velocity at the turning point (a periastron). Since the turning point is determined by the orbital parameter, there exists a dependence of the gravitational wave on particle spin. We find that the total energy of l=2 gravitational waves gets larger as the spin increases in the antiparallel direction to the orbital angular momentum. For an ultracompact star, in addition to such an orbital contribution, we find the quasinormal modes excited by a scattered particle, whose excitation rate to gravitational waves depends on the particle spin. We also discuss the ratio of the total angular momentum to the total energy of gravitational waves and explain its spin dependence.

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Published date: June 2001

Identifiers

Local EPrints ID: 29407
URI: http://eprints.soton.ac.uk/id/eprint/29407
ISSN: 1550-7998
PURE UUID: 33ed557e-0fd9-4441-87bf-5cc1b73789e8

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Date deposited: 12 May 2006
Last modified: 15 Mar 2024 07:31

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Contributors

Author: Kazuhiro Tominaga
Author: Motoyuki Saijo
Author: Kei-ichi Maeda

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