2D numerical study for magnetic field dependence of neutrino-driven core-collapse supernova models
2D numerical study for magnetic field dependence of neutrino-driven core-collapse supernova models
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DOI：
10.1093/mnras/staa3095
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发表时间：
2020-08
影响因子：
4.8
通讯作者：
J. Matsumoto;T. Takiwaki;K. Kotake;Y. Asahina;H. R. Takahashi
中科院分区：
文献类型：
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作者：
J. Matsumoto;T. Takiwaki;K. Kotake;Y. Asahina;H. R. Takahashi
我们研究了磁场对非旋转恒星内核动力学的影响，通过进行二维（2D），磁流体动力学（MHD）模拟。为此，我们已经更新了我们的中微子辐射流体动力学超新星代码，包括MHD采用的发散清洗方法与有限体积和面积重建的仔细治疗。通过改变磁场的初始强度，研究了15.0、18.4和27.0 M\odot前超新星祖先的演化。在我们的研究中，一个有趣的发现是中微子驱动的爆炸发生与初始磁场的强度无关。对于在这项工作中提出的2D模型，中微子加热是爆炸的主要驱动力，而磁场次要有助于爆炸前的动力学。结果表明，在小尺度下，强磁场对中微子驱动湍流的增长有一定的抑制作用。这导致在激波后区域的湍流动能的缓慢增加，导致较强的初始磁场的模型的激波复苏的稍微延迟的发病。
We study the effects of the magnetic field on the dynamics of non-rotating stellar cores by performing two-dimensional (2D), magnetohydrodynamics (MHD) simulations. To this end, we have updated our neutrino-radiation-hydrodynamics supernova code to include MHD employing a divergence cleaning method with both careful treatments of finite volume and area reconstructions. By changing the initial strength of the magnetic field, the evolution of $15.0$, $18.4$ and $27.0$ $M_\odot$ presupernova progenitors is investigated. An intriguing finding in our study is that the neutrino-driven explosion occurs regardless of the strength of the initial magnetic field. For the 2D models presented in this work, the neutrino heating is the main driver for the explosion, whereas the magnetic field secondary contributes to the pre-explosion dynamics. Our results show that the strong magnetic field weakens the growth of the neutrino-driven turbulence in the small scale compared to the weak magnetic field. This results in the slower increase of the turbulent kinetic energy in the postshock region, leading to the slightly delayed onset of the shock revival for models with the stronger initial magnetic field.