Magnetic support for neutrino-driven explosion of 3D non-rotating core-collapse supernova models
Magnetic support for neutrino-driven explosion of 3D non-rotating core-collapse supernova models
复制标题
3D非旋转核心塌陷超新星模型中微子驱动爆炸的磁力支持
DOI：
10.1093/mnras/stac2335
复制
发表时间：
2022
影响因子：
4.8
通讯作者：
Takahashi Hiroyuki R.
中科院分区：
文献类型：
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作者：
Matsumoto Jin;Takiwaki Tomoya;Kotake Kei;Asahina Yuta;Takahashi Hiroyuki R.
通过对光谱中微子输运的三维磁流体动力学模拟，研究了磁场对非旋转恒星核反弹后超新星动力学的影响。本文比较了20和27兆超新星前祖星的强磁化和弱磁化模型的爆炸性。我们发现，虽然在增益区的中微子加热到湍流能量，包括磁场的转换效率是没有显着不同的强，弱场模型之间，放大的磁场，由于中微子驱动的对流大的热气泡只是落后于失速冲击的结果在一个更快，更有活力的爆炸在强磁化模型。此外，通过比较强场模型中27 M中微子前身体模拟的二阶和五阶空间精度的差异，我们还发现，空间上的高阶精度对爆炸有利，因为它增强了增益区中微子驱动对流的增长。基于非旋转模型的核塌缩超新星模拟结果，提出了质子中子星星（PNS）磁场起源的一种新的可能性。在PNS表面附近的对流稳定壳层中，磁场被积累和放大到磁星水平，即G。
The impact of the magnetic field on post-bounce supernova dynamics of non-rotating stellar cores is studied by performing 3D magnetohydrodynamics simulations with spectral neutrino transport. The explodability of strongly and weakly magnetized models of 20 and 27 M⊙pre-supernova progenitors are compared. We find that although the efficiency for the conversion of the neutrino heating into turbulent energy including magnetic fields in the gain region is not significantly different between the strong and weak field models, the amplified magnetic field due to the neutrino-driven convection on large hot bubbles just behind stalled shock results in a faster and more energetic explosion in the strongly magnetized models. In addition, by comparing the difference between the 2nd- and 5th-order spatial accuracy of the simulation in the strong field model for 27 M⊙progenitor, we also find that the higher order accuracy in space is beneficial to the explosion because it enhances the growth of neutrino-driven convection in the gain region. Based on our results of core-collapse supernova simulations for the non-rotating model, a new possibility for the origin of the magnetic field of the protoneutron star (PNS) is proposed. The magnetic field is accumulated and amplified to magnetar level, that is,G, in the convectively stable shell near the PNS surface.