Gravitational Radiation from Axisymmetric Rotational Core Collapse
Gravitational Radiation from Axisymmetric Rotational Core Collapse
复制标题
轴对称旋转核心塌陷的引力辐射
DOI：
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发表时间：
2003
期刊：
影响因子：
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通讯作者：
Katsuhiko Sato
中科院分区：
文献类型：
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作者：
K. Kotake;S. Yamada;Katsuhiko Sato
我们对轴对称超新星核心的旋转坍缩进行了一系列二维流体动力学模拟。我们采用一个现实的状态方程（EOS），并考虑到电子捕获和中微子输运的所谓泄漏计划。将真实状态方程与微观物理相结合应用于二维模拟计算转动核坍缩中的引力辐射是重要的一步。我们利用四极公式计算了牛顿引力下引力波的振幅和波形。通过这些计算，我们扩展了引力波形的传统类别。我们的研究结果表明，引力波的峰值振幅大多是在灵敏度范围内的激光干涉仪，如TAMA和第一个LIGO的源在10千秒差距。此外，我们发现，第二个峰值的振幅是在第一个LIGO的检测极限的来源，并首先指出检测的重要性，因为它会给我们的信息，演化的大质量恒星的角动量分布。
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.