THE HADRONIC ORIGIN OF THE HARD GAMMA-RAY SPECTRUM FROM BLAZAR 1ES 1101-232
THE HADRONIC ORIGIN OF THE HARD GAMMA-RAY SPECTRUM FROM BLAZAR 1ES 1101-232
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DOI：
10.1088/0004-637x/783/2/108
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发表时间：
2014-01
期刊：
影响因子：
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通讯作者：
G. Cao;Jian-cheng Wang
中科院分区：
文献类型：
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作者：
G. Cao;Jian-cheng Wang
来自遥远耀变体的非常硬的γ射线谱挑战了传统的同步辐射自康普顿（SSC）模型，这可能表明除了SSC发射之外还有额外的高能成分的贡献。本文研究了来自遥远耀变体的硬γ射线谱的可能来源。我们发展了一个解释blazar 1 ES 1101-232硬γ射线谱的模型。在该模型中，光学和X射线辐射将来自初级电子和次级对的同步辐射，GeV发射将由SSC过程产生，然而，硬γ射线谱将来自通过质子-光子相互作用产生的中性π的衰变。与喷流内的同步辐射光子。我们的模型能很好地解释1 ES 1101-232的观测谱能量分布，特别是很硬的γ能谱。然而，我们的模型需要非常大的质子功率才能通过质子-光子相互作用有效地产生γ射线。
The very hard γ-ray spectrum from distant blazars challenges the traditional synchrotron self-Compton (SSC) model, which may indicate that there is a contribution from an additional high-energy component beyond the SSC emission. In this paper, we study the possible origin of the hard γ-ray spectrum from distant blazars. We develop a model to explain the hard γ-ray spectrum from blazar 1ES 1101-232. In the model, the optical and X-ray radiation would come from the synchrotron radiation of primary electrons and secondary pairs and the GeV emission would be produced by the SSC process, however, the hard γ-ray spectrum would originate from the decay of neutral pion produced through proton–photon interactions with the synchrotron radiation photons within the jet. Our model can explain the observed spectral energy distribution of 1ES 1101-232 well, especially the very hard γ-ray spectrum. However, our model requires a very large proton power to efficiently produce the γ-ray through proton–photon interactions.