标题： 关于旋转驱动脉冲星与脉泽星云的耦合 显示英文标题

标题： On the Coupling of Rotation Powered Pulsars to Plerionic Nebulae

摘要： 在讨论了蟹状脉冲星与蟹状星云之间MHD风耦合的观测限制后，回顾并应用了横向相对论性激波结构理论，以解释星云中的丝状结构作为分布风终止激波结构的表现，其能量主要由在脉冲星旋转赤道加速到与脉冲星开放磁场线总电压相当的能量的重离子主导，并携带与Goldreich-Julian电流相当的电流。 介绍了关于激波结构变化的新结果，这些结果表明，回旋的离子团块发出向外传播的有限振幅压缩波，这与最近的地基观测结果一致。 简要讨论了该理论对X射线、$\gamma$-射线和高能中微子辐射的影响，以及上游风中磁能密度低的问题和星云射电辐射的起源问题。 对其他类似天体的简要讨论得出结论，在这些系统能够像蟹状星云那样被建模之前，需要更详细的观测。 显示英文摘要

摘要： After discussion of observational constraints on the nature of the MHD wind coupling between the Crab Pulsar and the Crab Nebula, the theory of transverse relativistic shock structure is reviewed and applied to the interpretation of the wisps in the Nebula as the manifestation of the distributed wind termination shock structure, energetically dominated by heavy ions, accelerated in the rotational equator of the pulsar to energies comparable to the total voltage across the pulsar's open field lines and carrying a current comparable to the Goldreich- Julian current. New results on the variability of the shock structure are presented, which show that the gyrating ion bunches emit outwardly traveling finite amplitude compressional waves, in agreement with recent ground based observations. The implications of the theory for X-ray, $\gamma$-ray and high energy neutrino emission are briefly discussed, as are the problems of low magnetic energy density in the upstream wind and the origin of the Nebular radio emission. A brief discussion of other plerions leads to the conclusion that much more detailed observations are needed before these systems can be modeled with the same sophistication as can be done for the Crab Nebula.