Three-dimensional simulations of rapidly rotating core-collapse supernovae: finding a neutrino-powered explosion aided by non-axisymmetric flows
Three-dimensional simulations of rapidly rotating core-collapse supernovae: finding a neutrino-powered explosion aided by non-axisymmetric flows
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DOI：
10.1093/mnrasl/slw105
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发表时间：
2016-02
影响因子：
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通讯作者：
T. Takiwaki;K. Kotake;Y. Suwa
中科院分区：
文献类型：
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作者：
T. Takiwaki;K. Kotake;Y. Suwa
采用中微子输运方案，在各向同性扩散源近似下，对11.2 $和27 $M_{/odot}$星进行了一系列三维转动核坍缩模拟.通过系统地改变转动的初始强度，我们发现27 $M_{/odot}$的前身核存在转动辅助的爆炸，但在没有转动的情况下，这种爆炸是失败的。在以前的二维（2D）自洽旋转模型中没有捕捉到的独特功能，因为不断增长的非轴对称不稳定性起着关键作用。在快速旋转的情况下，由所谓的低$T/|W| $不稳定性增强了从原中子星星（PNS）到增益区的能量输运，使激波膨胀更有能量。爆炸在垂直于旋转轴的方向上发生得更强烈，这与以前的2D预测不同。
We report results from a series of three-dimensional (3D) rotational core-collapse simulations for $11.2$ and 27 $M_{/odot}$ stars employing neutrino transport scheme by the isotropic diffusion source approximation. By changing the initial strength of rotation systematically, we find a rotation-assisted explosion for the 27$M_{/odot}$ progenitor, which fails in the absence of rotation. The unique feature was not captured in previous two-dimensional (2D) self-consistent rotating models because the growing non-axisymmetric instabilities play a key role. In the rapidly rotating case, strong spiral flows generated by the so-called low $T/|W|$ instability enhance the energy transport from the proto-neutron star (PNS) to the gain region, which makes the shock expansion more energetic. The explosion occurs more strongly in the direction perpendicular to the rotational axis, which is different from previous 2D predictions.