MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE IN THREE DIMENSIONS
MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE IN THREE DIMENSIONS
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三个维度的磁旋转核心塌陷超新星
DOI：
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发表时间：
2014
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通讯作者：
E. Schnetter
中科院分区：
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作者：
P. Mösta;S. Richers;C. Ott;R. Haas;A. Piro;K. Boydstun;E. Abdikamalov;C. Reisswig;E. Schnetter
我们提出了新的三维（3D）广义相对论磁流体动力学模拟的快速旋转强磁化核心崩溃的结果。这些模拟是第一次，包括一个微物理有限温度状态方程和泄漏计划，捕捉整体能量和轻子数交换由于反弹后中微子发射。我们的研究结果表明，磁旋转核心坍缩超新星的3D动力学是从根本上不同的轴对称（2D）以前的模拟的基础上所预期的。一个强大的双极喷流，在一个模拟约束到2D是削弱了螺旋不稳定性和失败，在全3D。虽然可能存在多个（磁）流体动力学不稳定性，我们的分析表明，射流被破坏的旋转轴附近的超强环形场的m = 1扭结不稳定性。代替轴对称射流，一个全新的，以前未报道的流动结构的发展。从核心喷出的高度磁化螺旋状等离子体漏斗将极区的激波挤出，形成了广泛的长期膨胀的波瓣。在反弹后185 ms的完整3D模拟结束时，我们没有观察到失控的爆炸。此时，叶瓣的最大半径已达10900公里。
We present results of new three-dimensional (3D) general-relativistic magnetohydrodynamic simulations of rapidly rotating strongly magnetized core collapse. These simulations are the first of their kind and include a microphysical finite-temperature equation of state and a leakage scheme that captures the overall energetics and lepton number exchange due to postbounce neutrino emission. Our results show that the 3D dynamics of magnetorotational core-collapse supernovae are fundamentally different from what was anticipated on the basis of previous simulations in axisymmetry (2D). A strong bipolar jet that develops in a simulation constrained to 2D is crippled by a spiral instability and fizzles in full 3D. While multiple (magneto-)hydrodynamic instabilities may be present, our analysis suggests that the jet is disrupted by an m = 1 kink instability of the ultra-strong toroidal field near the rotation axis. Instead of an axially symmetric jet, a completely new, previously unreported flow structure develops. Highly magnetized spiral plasma funnels expelled from the core push out the shock in polar regions, creating wide secularly expanding lobes. We observe no runaway explosion by the end of the full 3D simulation 185 ms after bounce. At this time, the lobes have reached maximum radii of ∼900 km.