GENERATION OF MAGNETIC FIELDS BY THE STATIONARY ACCRETION SHOCK INSTABILITY
GENERATION OF MAGNETIC FIELDS BY THE STATIONARY ACCRETION SHOCK INSTABILITY
复制标题
静止吸积激波不稳定性产生磁场
DOI：
10.1088/0004-637x/713/2/1219
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发表时间：
2008
期刊：
影响因子：
--
通讯作者：
A. Mezzacappa
中科院分区：
文献类型：
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作者：
E. Endeve;C. Cardall;R. Budiardja;A. Mezzacappa
我们开始探索静止吸积激波不稳定性（SASI）产生磁场的能力，方法是在最初的球对称流体配置中添加一个弱的、静止的、径向（但双极）磁场，在某些情况下还添加旋转，该流体配置模拟了反弹后超新星环境中的失速激波。在轴对称模拟中，我们发现流入和流出极地的纬向流动的循环放大了平行于对称轴的磁场，通常使总磁能增加约 2 个数量级。非轴对称计算会导致根本不同的流动和更大的磁能增加：与 SASI 螺旋模式相关的剪切有助于形成广泛的湍流场放大机制，将磁能提高近 4 个数量级（这一结果对数值模拟的空间分辨率仍然非常敏感）。虽然 SASI 可能有助于中子星磁化，但这些模拟并未显示由于 SASI 引起的磁场放大而引起的激波整体演化的定性新特征。
We begin an exploration of the capacity of the stationary accretion shock instability (SASI) to generate magnetic fields by adding a weak, stationary, and radial (but bipolar) magnetic field, and in some cases rotation, to an initially spherically symmetric fluid configuration that models a stalled shock in the post-bounce supernova environment. In axisymmetric simulations, we find that cycles of latitudinal flows into and radial flows out of the polar regions amplify the field parallel to the symmetry axis, typically increasing the total magnetic energy by about 2 orders of magnitude. Non-axisymmetric calculations result in fundamentally different flows and a larger magnetic energy increase: shearing associated with the SASI spiral mode contributes to a widespread and turbulent field amplification mechanism, boosting the magnetic energy by almost 4 orders of magnitude (a result which remains very sensitive to the spatial resolution of the numerical simulations). While the SASI may contribute to neutron star magnetization, these simulations do not show qualitatively new features in the global evolution of the shock as a result of SASI-induced magnetic field amplification.
DOI：
10.1088/0004-637x/694/1/664
发表时间：
2007-08
期刊：
The Astrophysical Journal
影响因子：
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作者：
A. Marek;H. Janka
通讯作者：
A. Marek;H. Janka