Computing gravitational waves from slightly nonspherical stellar collapse to black hole: Odd-parity perturbation

Details Computing gravitational waves from slightly nonspherical stellar collapse to black hole: Odd-parity perturbation Computing gravitational waves from slightly nonspherical stellar collapse to black hole: Odd-parity perturbation

2003-05-15

arxiv.org/abs/gr-qc/0305058v2

Phys.Rev.D68:024002,2003

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

31 pages, accepted for publication in Phys. Rev. D, typos and minor errors corrected

Scientific paper

10.1103/PhysRevD.68.024002

Nonspherical stellar collapse to a black hole is one of the most promising gravitational wave sources for gravitational wave detectors. We numerically study gravitational waves from a slightly nonspherical stellar collapse to a black hole in linearized Einstein theory. We adopt a spherically collapsing star as the zeroth-order solution and gravitational waves are computed using perturbation theory on the spherical background. In this paper we focus on the perturbation of odd-parity modes. Using the polytropic equations of state with polytropic indices $n_p=1$ and 3, we qualitatively study gravitational waves emitted during the collapse of neutron stars and supermassive stars to black holes from a marginally stable equilibrium configuration. Since the matter perturbation profiles can be chosen arbitrarily, we provide a few types for them. For $n_p=1$, the gravitational waveforms are mainly characterized by a black hole quasinormal mode ringing, irrespective of perturbation profiles given initially. However, for $n_p=3$, the waveforms depend strongly on the initial perturbation profiles. In other words, the gravitational waveforms strongly depend on the stellar configuration and, in turn, on the ad hoc choice of the functional form of the perturbation in the case of supermassive stars.

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