标题： 高能脉冲的风模型 显示英文标题

标题： A wind model for high energy pulses

摘要： σ问题的一个解——即寻找一种能够在脉冲星风中将Poynting能流转换为粒子携带能流的机制——几年前由Coroniti和Michel提出，他们考虑了条纹风中磁重联的特定方案。后来证明这个方案是无效的。本文讨论了重联过程的基本微观物理，并得出结论认为更快速的重联方案是可以接受的。假设重联从光筒之外某处开始耗散，我们计算了由此产生的辐射特征，发现被加热粒子的同步辐射通常表现出周期性，一般显示脉冲和间脉冲两种特性。对于蟹状星云和波江座星云脉冲星，这些预测的间隔与观测结果非常吻合。使用适合蟹状星云脉冲星的参数——光筒处的磁化参数σL=6×10^4，洛伦兹因子Γ=250——与观测到的总脉冲亮度合理一致。这表明年轻脉冲星的高能脉冲并非起源于光筒内的共转磁层（这是所有其他模型中的情况），而是来自光筒外径向方向的风。 显示英文摘要

摘要： A solution to the sigma problem - that of finding a mechanism capable of converting Poynting energy flux to particle-borne energy flux in a pulsar wind - was proposed several years ago by Coroniti and Michel who considered a particular prescription for magnetic reconnection in a striped wind. This prescription was later shown to be ineffective. In this paper, we discuss the basic microphysics of the reconnection process and conclude that a more rapid prescription is permissible. Assuming dissipation to set in at some distance outside the light-cylinder, we compute the resulting radiation signature and find that the synchrotron emission of heated particles appears periodic, in general showing both a pulse and an interpulse. The predicted spacing of these agrees well with observation in the case of the Crab and Vela pulsars. Using parameters appropriate for the Crab pulsar - magnetization parameter at the light cylinder sigma_L = 6 x 10^4, Lorentz factor Gamma=250 - reasonable agreement is found with the observed total pulsed luminosity. This suggest that the high-energy pulses from young pulsars originate not in the co-rotating magnetosphere within the light cylinder (as in all other models) but from the radially directed wind well outside it.