在甚高能段(E>100 GeV)观测到的河外TeV 伽玛射线源有50个，这些源中大部分源是耀变体。轻子起源模型与河外星系背景光模型预言观测到的耀变体源初高能伽玛射线辐射能谱应该表现出明显的吸收特征。然而，高能辐射探测器却观测到TeV耀变体伽玛射线能段存在较硬的内禀谱。上述观测结果表明可能在源外存在其它高能伽玛射线光子产生过程。本项目拟研究耀变体加速产生的高能宇宙线质子与河外星系背景光光子、宇宙微波背景光光子相互作用(pγ相互作用)产生的电磁级联过程，以及源内高能伽玛光子与河外星系背景光光子相互作用产生的正负电子对通过逆康普顿散射过程上散射宇宙微波背景光子产生的次级伽玛射线辐射，确定TeV 耀变体次级伽玛光子对高能伽玛射线辐射能谱的贡献，解决TeV 耀变体高能伽玛射线辐射"硬谱"的起源。同时，利用TeV 耀变体高能伽玛射线辐射"硬谱"限定星际磁场和预测宇宙中微子产生。

Most of the 50 extragalactic TeV gamma rays sources, which are observated in the very high energy gamma rays (E>100 GeV) band，are Blazars. Lepton model and extragalactic background light (EBL) model predicted that the primary gamma rays should exhibit clear signatures of absorption. However, in the TeV energy bands, the observation shows the hard intrinsic spectrum. This suggests that there is probable the process of production of secondary gamma ray photons outside the source. The propose aims at the secondary gamma ray photons production, where the photons are produced the cascade initiated by the high energic cosmic rays protons that are accelerated by distant Blazars, interaction with ectragalactic background light (EBL) photons and cosmic microwave background (CMB) photons, and inverse Compton up scattering the CMB photons initiated by the pairs production due to TeV gamma ray photons interactions with EBL. Then, the secondary gamma ray photons contribution for the high energy gamma ray spectra should be confirmed,and we expect that the secondary gamma ray photons can be as a origin of the hard intrinsic spectrum from TeV blazars. Otherwise, the intergalactic magnetic fields (IGMF) can be determinated and the cosmic neutrino production can be predicted by the model results that are obtained by fitting the hard intrinsic high spectra data from TeV blazars.