Confinement of the Crab pulsar's wind by its supernova remnant
Confinement of the Crab pulsar's wind by its supernova remnant
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DOI：
10.1086/162356
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发表时间：
1984-08
期刊：
影响因子：
--
通讯作者：
C. Kennel;F. Coroniti
中科院分区：
文献类型：
--
作者：
C. Kennel;F. Coroniti
我们建立了一个稳定状态，球对称，磁流体动力学模型的蟹状星云。一个高度相对论性的正子脉冲星风被一个强大的MHD激波终止，该激波使气流减速并增加其压力，以匹配最近发现的围绕星云的超新星遗迹所施加的边界条件。如果冲击波上游脉冲星风的磁光度大约是其粒子光度的0.3%，则由残余物施加的压力和速度边界条件将冲击波置于我们推断的位置;靠近脉冲星周围观测到的欠亮区域的外边界。为了满足边界条件和自洽地计算星云同步辐射，必须考虑风的弱磁化。
We construct a steady state, spherically symmetric, magnetohydrodynamic model of the Crab nebual. A highly relativistic, positronic pulsar wind is terminated by a strong MHD shock that decelerates the flow and increases its pressure to match boundary conditions imposed by the recently discovered supernova remnant that surrounds the nebula. If the magnetic luminosity of the pulsar wind upsteam of the shock is about 0.3% of its particle luminosity, the pressure and velocity boundary conditions imposed by the remnant place the shock where we infer it to be; near the outer boundary of an underluminous region observed to surround the pulsar. It is necessary to include the weak magnetization of the wind to satisfy the boundary conditions and to calculate the nebular synchrotron radiation self-consistently.