PWNe与分子云相互作用的Gamma-Ray辐射
Gamma-Ray Emission from PWNe Interacting with Molecular Clouds
摘要：
我们考虑的情况下，脉冲星（和它的星云）是内部或接近分子云的高密度区域形成的。我们应用最近的脉冲星风星云（PWN），其中不仅包括由于注入轻子辐射过程，但也由于注入相对论性强子的过程，以计算预期的伽马射线发射从这样的相互作用PWNe的伽马射线辐射模型。已经对两个这种类型的物体进行了示例计算，从这两个物体最近观察到TeV伽马射线源（IC 443和W 41）。我们表明，γ射线辐射低于几个TeV可以产生轻子加速在过去的附近的星系。能量超过10 TeV的伽马射线可以由强子与超新星遗迹内的物质和周围的致密云相互作用产生。与低能量TeV辐射相反，这种高能量TeV辐射应该与能够捕获强子的致密云的位置相关，因为它们具有强磁场。
英文摘要：
We consider a situation in which a pulsar (and its nebula) is formed inside or close to a high density regions of a molecular cloud. We apply a recent model for the gamma radiation of pulsar wind nebulae (PWN), which includes not only radiation processes due to injected leptons but also processes due to injection of relativistic hadrons, in order to calculate the expected gamma-ray emission from such interacting PWNe. The example calculations have been performed for two objects of this type from which directions TeV gamma-ray sources have recently been observed (IC443 and W41). We show that the gamma-ray emission below a few TeV can be produced by leptons accelerated in the past in the vicinity of the pulsars. gamma-rays with energies above ~10 TeV can be produced by hadrons interacting with the matter inside the supernova remnant and surrounding dense clouds. In contrary to the low energy TeV emission, this high energy TeV emission should be correlated with the location of dense clouds able to capture hadrons due to their strong magnetic fields.
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