Magnetorotational supernovae
Magnetorotational supernovae
复制标题
磁转超新星
DOI：
10.1111/j.1365-2966.2005.08888.x
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发表时间：
2004
期刊：
影响因子：
--
通讯作者：
Kurt W. Weiler
中科院分区：
文献类型：
--
作者：
S. Moiseenko;G. Bisnovatyi;S. Immler;Kurt W. Weiler
我们提出了一个超新星爆炸的磁旋转模型的二维模拟结果。核心坍缩后，核心由快速旋转的原中子星星和径向旋转的包层组成。在磁场演化的初始阶段，由逆时针旋转产生的磁能的环形部分随时间线性增长。磁流体动力学不稳定性的发展终止了环形磁场的线性增长，导致磁能增长急剧加速。当磁压变得与原中子星星外围距离星星中心约10 − 15 km处的气压相当时，MHD压缩波出现并穿过坍缩铁芯的包层。它很快转变为快速的MHD冲击波，并产生超新星爆炸。我们的模拟给出了爆炸的能量为0。6 · 10 51尔格。爆炸喷出的质量是1000。14英里采用基于拉格朗日三角形变结构网格的隐式数值方法进行数值模拟。
We present the results of 2D simulations of the magnetorotational model of a supernova explosion. After the core collapse the core consists of rapidly a rotating proto-neutron star and a differentially rotating envelope. The toroidal part of the magnetic energy generated by the differential rotation grows linearly with time at the initial stage of the evolution of the magnetic field. The linear growth of the toroidal magnetic field is terminated by the development of magnetohydrodynamic instability, leading to drastic acceleration in the growth of magnetic energy. At the moment when the magnetic pressure becomes comparable with the gas pressure at the periphery of the proto-neutron star ∼ 10 − 15km from the star centre the MHD compression wave appears and goes through the envelope of the collapsed iron core. It transforms soon to the fast MHD shock and produces a supernova explosion. Our simulations give the energy of the explosion 0 . 6 · 10 51 ergs. The amount of the mass ejected by the explosion is ∼ 0 . 14 M ⊙ . The implicit numerical method, based on the Lagrangian triangular grid of variable structure, was used for the simulations.