Scattering of cosmic rays by magnetohydrodynamic interstellar turbulence.
Scattering of cosmic rays by magnetohydrodynamic interstellar turbulence.
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DOI：
10.1103/physrevlett.89.281102
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发表时间：
2002-05
影响因子：
8.6
通讯作者：
Huirong Yan;A. Lazarian
中科院分区：
文献类型：
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作者：
Huirong Yan;A. Lazarian
磁流体动力学（MHD）湍流的最新进展要求我们对宇宙线输运的理解进行实质性的修正。我们使用最近获得的标度的MHD模式来计算宇宙线的散射频率。我们考虑磁流体模式（Alfvénic，慢，快）和渡越时间阻尼快模式的陀螺共振。我们的结论是，与快模式的回旋共振是占主导地位的贡献，宇宙射线散射的典型星际条件。与早期的研究相比，我们发现Alfvénic和慢模式是低效的，因为它们远离通常假设的各向同性。
Recent advances in understanding of magnetohydrodynamic (MHD) turbulence call for substantial revisions in our understanding of cosmic ray transport. We use recently obtained scalings of MHD modes to calculate the scattering frequency for cosmic rays. We consider gyroresonance with MHD modes (Alfvénic, slow, and fast) and transit-time damping by fast modes. We conclude that the gyroresonance with fast modes is the dominant contribution to cosmic ray scattering for the typical interstellar conditions. In contrast to earlier studies, we find that Alfvénic and slow modes are inefficient because they are far from the isotropy usually assumed.