论文标题
螃蟹星云辐射的湍流模型
Turbulent model of Crab nebula radiation
论文作者
论文摘要
我们构建了螃蟹星云的非热发射的湍流模型。目前的模型解决了狗窝-Coroniti（1984）模型的许多长期问题：（i）Sigma问题； （ii）无线电电子的硬光谱； （iii）伽马射线耀斑的高峰值能量； （IV）和红外发射的空间演化。星云包含两个注入的颗粒人群：通过FERMI-I机制在风终止冲击下加速的组件I，并且在重新连接高度磁化（$σ$ \ gg 1 $）等离子体的湍流中，组件II加速了。重新连接的湍流组件-II从无线电延伸到伽玛射线：它以硬光谱加速无线电电子，破坏大型磁通量（从而解决Sigma-Promlem），并有时会产生伽马射线弹性（来自最大规模重新连接事件）。该模型重现了蟹状星云的宽带光谱，从无线电中的低频同步加速器发射到TEV能量处的反孔子发射，以及IR和光条带的光谱指数的空间分辨演化。
We construct a turbulent model of the Crab Nebula's non-thermal emission. The present model resolves a number of long-standing problems of the Kennel-Coroniti (1984) model: (i) the sigma problem; (ii) the hard spectrum of radio electrons; (iii) the high peak energy of gamma-ray flares; (iv) and the spacial evolution of the infrared (IR) emission. The Nebula contains two populations of injected particles: Component-I accelerated at the wind termination shock via Fermi-I mechanism, and Component-II accelerated in reconnecting turbulence in highly magnetized ($σ$ $\gg 1$) plasma in the central part of the Crab Nebula. The reconnecting turbulence Component-II extends from radio to gamma rays: it accelerate radio electrons with a hard spectrum, destroy the large scale magnetic flux (and thus resolves the sigma-problem), and occasionally produces gamma-ray flares (from the largest scale reconnection events). The model reproduces the broad-band spectrum of the Crab Nebula, from low-frequency synchrotron emission in radio to inverse-Compton emission at TeV energies, as well as spatially resolved evolution of the spectral indices in IR and optical bands.
