The Origin of the Magnetic Field and Relativistic Particles in the Crab Nebula
The Origin of the Magnetic Field and Relativistic Particles in the Crab Nebula
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DOI：
10.1093/mnras/167.1.1
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发表时间：
1974-04
影响因子：
4.8
通讯作者：
M. Rees;J. Gunn
中科院分区：
文献类型：
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作者：
M. Rees;J. Gunn
来自蟹状星云脉冲星NP 0531的能量可能部分以30 Hz波的形式出现，部分以包含环形磁场的相对论风的形式出现。在相对论外流的压力与星云内的压力平衡的地方，预计会出现激波不连续。这种冲击将发生在半径Rs处，它大约是星云总半径Rneb的10%。相对论粒子和磁通量将在区域Rs <R<Rneb中积累。这个区域的磁场会逐渐增强到均分强度，即使这个磁场只包含脉冲星流出的相对论能量的百分之几。30赫兹的波会被吸收到R R，它们的能量被转移到相对论电子。星云主体的连续光谱将完全是同步辐射。这个模型的相关性，各种观测到的蟹状星云的功能进行了简要的探讨。
The power from the Crab Pulsar NP 0531 probably emerges partly as 30 Hz waves and partly as a relativistic wind containing a toroidal magnetic field. A shock discontinuity is expected where the pressure of the relativistic outflow balances the pressure within the nebula. This shock would occur at a radiusRswhich is about 10 per cent of the total nebular radiusRneb. The relativistic particles and the magnetic flux would accumulate in the regionRs<R<Rneb. The magnetic field in this region would build up to equipartition strength, even if this field embodied only a few per cent of the relativistic energy outflow from the pulsar. The 30 Hz waves would be absorbed atR≃Rs, their energy being transferred to relativistic electrons. The continuum from the bulk of the nebula would then be entirely synchrotron radiation. The relevance of this model to various observed features of the Crab Nebula is briefly explored.