The inner knot of the Crab nebula
The inner knot of the Crab nebula
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蟹状星云的内结
DOI：
10.1093/mnras/stv2570
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发表时间：
2015
影响因子：
4.8
通讯作者：
O. Porth
中科院分区：
文献类型：
--
作者：
M. Lyutikov;S. Komissarov;O. Porth
我们将蟹状星云的内结模拟为来自相对论脉冲星风的非球形MHD终止激波的同步辐射。激波后的流动是温和的相对论性的，因此，多普勒波束对激波的外观有很大的影响。该模型可以再现纽结的位置、大小、伸长、亮度分布、光度和偏振，只要产生纽结的脉冲星风截面的有效磁化强度较低（σ ≤ 1）。在条纹风模型中，这意味着条纹区相当宽，蟹状星云脉冲星的磁倾角≥45°;这与先前基于脉冲星伽马射线发射的模型相关估计一致。我们的结论是，微小的结确实是一个亮点的表面上的准静态磁相对论冲击，这个冲击是一个网站的有效粒子加速。另一方面，推导出的低磁化的结等离子体意味着这是一个不太可能的网站螃蟹的伽马射线耀斑，如果它们与快速相对论磁重联事件。
We model the inner knot of the Crab nebula as a synchrotron emission coming from the non-spherical MHD termination shock of relativistic pulsar wind. The post-shock flow is mildly relativistic; as a result the Doppler beaming has a strong impact on the shock appearance. The model can reproduce the knot location, size, elongation, brightness distribution, luminosity and polarization provided the effective magnetization of the section of the pulsar wind producing the knot is low, σ ≤ 1. In the striped wind model, this implies that the striped zone is rather wide, with the magnetic inclination angle of the Crab pulsar ≥45°; this agrees with the previous model-dependent estimate based on the gamma-ray emission of the pulsar. We conclude that the tiny knot is indeed a bright spot on the surface of a quasi-stationary magnetic relativistic shock and that this shock is a site of efficient particle acceleration. On the other hand, the deduced low magnetization of the knot plasma implies that this is an unlikely site for the Crab's gamma-ray flares, if they are related to the fast relativistic magnetic reconnection events.
影响因子：
4.8
作者：
S. Komissarov
通讯作者：
S. Komissarov