The Effect of Neutrino Radiation on Magnetorotational Instability in Proto-Neutron Stars
The Effect of Neutrino Radiation on Magnetorotational Instability in Proto-Neutron Stars
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DOI：
10.1086/509799
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发表时间：
2006-10
期刊：
影响因子：
--
通讯作者：
Y. Masada;T. Sano;K. Shibata
中科院分区：
文献类型：
--
作者：
Y. Masada;T. Sano;K. Shibata
中微子辐射在原中子星（PNS）的动量、热量和轻子传输中发挥着重要作用。这些扩散过程影响 PNS 中磁旋转不稳定性 (MRI) 的增长。我们对轴对称和非轴对称 MRI 进行局部线性分析，包括中微子输运和欧姆耗散的影响。我们发现，即使在中微子负载的PNS 中实现的多重扩散情况下，MRI 也能增长。当环形磁性成分超过极向磁性成分时，非轴对称 MRI 模式的增长速度比轴对称模式快得多。这些结果表明非轴对称 MRI 在 PNS 中的重要性。因此，了解MRI的三维非线性演化对于揭示核心塌陷超新星的爆炸机制是必要的。
Neutrino radiation takes a major role in the momentum, heat, and lepton transports in proto-neutron stars (PNSs). These diffusive processes affect the growth of the magnetorotational instability (MRI) in PNSs. We perform a local linear analysis for the axisymmetric and nonaxisymmetric MRI including the effects of neutrino transport and ohmic dissipation. We find that the MRI can grow even in the multidiffusive situations that are realized in neutrino-loaded PNSs. When the toroidal magnetic component dominates over the poloidal one, nonaxisymmetric MRI modes grow much faster than axisymmetric modes. These results suggest the importance of the nonaxisymmetric MRI in PNSs. Thus, understanding the three-dimensional nonlinear evolution of the MRI is necessary for revealing the explosion mechanism of core-collapse supernovae.