Abstract
We perform a series of two-dimensional hydrodynamic simulations of the rotational collapse of a supernova core in axisymmetry. We employ a realistic equation of state (EOS) and take into account electron, capture and neutrino transport by the so-called leakage scheme. It is an important step to apply the realistic EOS coupled with microphysics to 2D simulations for computing gravitational radiation in rotational core collapse. We use the quadrupole formula to calculate the amplitudes and the waveforms of the gravitational wave assuming Newtonian gravity. With these computations, we extend the conventional category of the gravitational waveforms. Our results show that the peak amplitudes of the gravitational wave are mostly within the sensitivity range of laser interferometers such as TAMA and the first LIGO for a source at a distance of 10 kpc. Furthermore, we find that the amplitudes of the second peaks are within the detection limit of the first LIGO for the source, and first point out the importance of the detection, since it will give us information as to the angular momentum distribution of evolved massive stars.
| Original language | English |
|---|---|
| Article number | 044023 |
| Pages (from-to) | 440231-440237 |
| Number of pages | 7 |
| Journal | Physical Review D - Particles, Fields, Gravitation and Cosmology |
| Volume | 68 |
| Issue number | 4 |
| Publication status | Published - 2003 Aug 15 |
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ASJC Scopus subject areas
- Physics and Astronomy(all)
- Nuclear and High Energy Physics
- Mathematical Physics
Cite this
Gravitational radiation from axisymmetric rotational core collapse. / Kotake, Kei; Yamada, Shoichi; Sato, Katsuhiko.
In: Physical Review D - Particles, Fields, Gravitation and Cosmology, Vol. 68, No. 4, 044023, 15.08.2003, p. 440231-440237.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Gravitational radiation from axisymmetric rotational core collapse
AU - Kotake, Kei
AU - Yamada, Shoichi
AU - Sato, Katsuhiko
PY - 2003/8/15
Y1 - 2003/8/15
N2 - We perform a series of two-dimensional hydrodynamic simulations of the rotational collapse of a supernova core in axisymmetry. We employ a realistic equation of state (EOS) and take into account electron, capture and neutrino transport by the so-called leakage scheme. It is an important step to apply the realistic EOS coupled with microphysics to 2D simulations for computing gravitational radiation in rotational core collapse. We use the quadrupole formula to calculate the amplitudes and the waveforms of the gravitational wave assuming Newtonian gravity. With these computations, we extend the conventional category of the gravitational waveforms. Our results show that the peak amplitudes of the gravitational wave are mostly within the sensitivity range of laser interferometers such as TAMA and the first LIGO for a source at a distance of 10 kpc. Furthermore, we find that the amplitudes of the second peaks are within the detection limit of the first LIGO for the source, and first point out the importance of the detection, since it will give us information as to the angular momentum distribution of evolved massive stars.
AB - We perform a series of two-dimensional hydrodynamic simulations of the rotational collapse of a supernova core in axisymmetry. We employ a realistic equation of state (EOS) and take into account electron, capture and neutrino transport by the so-called leakage scheme. It is an important step to apply the realistic EOS coupled with microphysics to 2D simulations for computing gravitational radiation in rotational core collapse. We use the quadrupole formula to calculate the amplitudes and the waveforms of the gravitational wave assuming Newtonian gravity. With these computations, we extend the conventional category of the gravitational waveforms. Our results show that the peak amplitudes of the gravitational wave are mostly within the sensitivity range of laser interferometers such as TAMA and the first LIGO for a source at a distance of 10 kpc. Furthermore, we find that the amplitudes of the second peaks are within the detection limit of the first LIGO for the source, and first point out the importance of the detection, since it will give us information as to the angular momentum distribution of evolved massive stars.
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M3 - Article
VL - 68
SP - 440231
EP - 440237
JO - Physical review D: Particles and fields
JF - Physical review D: Particles and fields
SN - 0556-2821
IS - 4
M1 - 044023
ER -