SUPERNOVA NEUTRINO LIGHT CURVES AND SPECTRA FOR VARIOUS PROGENITOR STARS: FROM CORE COLLAPSE TO PROTO-NEUTRON STAR COOLING
SUPERNOVA NEUTRINO LIGHT CURVES AND SPECTRA FOR VARIOUS PROGENITOR STARS: FROM CORE COLLAPSE TO PROTO-NEUTRON STAR COOLING
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DOI：
10.1088/0067-0049/205/1/2
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发表时间：
2012-10
期刊：
影响因子：
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通讯作者：
K. Nakazato;K. Sumiyoshi;H. Suzuki;T. Totani;H. Umeda;S. Yamada
中科院分区：
文献类型：
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作者：
K. Nakazato;K. Sumiyoshi;H. Suzuki;T. Totani;H. Umeda;S. Yamada
我们提出了一系列新的超新星中微子光曲线和光谱，通过数值模拟计算了各种祖恒星质量（13-50 M☉）和金属丰度（Z = 0.02和0.004），这将有助于广泛的超新星中微子研究，例如，模拟未来的中微子爆发探测地下探测器或对遗迹超新星中微子背景的理论预测。为了跟踪从坍缩开始到核心弹跳后20 s的演化过程，我们将早期的中微子辐射流体动力学模拟结果和后期中微子扩散的准静态演化计算结果结合起来，并将不同的激波恢复时间作为一个参数，该参数应取决于尚未知的爆炸机制。介绍了计算方法和基本结果，包括对祖模型的依赖和冲击恢复时间。中微子数据可以通过电子方式公开获取。
We present a new series of supernova neutrino light curves and spectra calculated by numerical simulations for a variety of progenitor stellar masses (13–50 M☉) and metallicities (Z = 0.02 and 0.004), which would be useful for a broad range of supernova neutrino studies, e.g., simulations of future neutrino burst detection by underground detectors or theoretical predictions for the relic supernova neutrino background. To follow the evolution from the onset of collapse to 20 s after the core bounce, we combine the results of neutrino-radiation hydrodynamic simulations for the early phase and quasi-static evolutionary calculations of neutrino diffusion for the late phase, with different values of shock revival time as a parameter that should depend on the still unknown explosion mechanism. We describe the calculation methods and basic results, including the dependence on progenitor models and the shock revival time. The neutrino data are publicly available electronically.