BLAZARS AS ULTRA-HIGH-ENERGY COSMIC-RAY SOURCES: IMPLICATIONS FOR TeV GAMMA-RAY OBSERVATIONS
BLAZARS AS ULTRA-HIGH-ENERGY COSMIC-RAY SOURCES: IMPLICATIONS FOR TeV GAMMA-RAY OBSERVATIONS
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DOI：
10.1088/0004-637x/749/1/63
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发表时间：
2011-07
期刊：
影响因子：
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通讯作者：
K. Murase;C. Dermer;H. Takami;G. Migliori
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文献类型：
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作者：
K. Murase;C. Dermer;H. Takami;G. Migliori
BL Lac天体和Fanaroff-Riley I射电星系的光谱通常用单带轻子同步自康普顿（SSC）模型来解释。相关的多波长数据的光谱建模给出了共动磁场强度，批量流出洛伦兹因子，和发射区域的大小。假设SSC模型的有效性，希拉斯条件表明，只有在极少数情况下，这样的源将质子加速到远高于1019 eV，因此如果由这种类型的射电大声活动星系核（AGN）提供动力，1020 eV的超高能宇宙射线（UHECR）很可能是重离子。核的生存被证明是可能的TeV BL拉克和错位对应弱光强子发射。强子产生的另一个特征是星系际UHECR诱导的级联辐射，这是对一些极端的不变耀变体（如1 ES 0229+200或1 ES 1101−232）的TeV光谱的另一种解释。我们研究这种级联信号，考虑到结构化的河外磁场中的源应嵌入的影响。我们证明了宇宙射线偏转对γ射线通量的重要性，并表明所需的绝对宇宙射线光度大于从UHECR观测推断的平均UHECR光度，甚至可以与超大质量黑洞的爱丁顿光度相媲美。未来使用切伦科夫望远镜阵列和高海拔水切伦科夫探测器阵列进行的TeV γ射线观测可以通过观测来自相对低红移源（如1 ES 0229+200）的>25 TeV光子和来自更遥远的射电噪声活动星系核的100 TeV光子来测试UHECR加速。
The spectra of BL Lac objects and Fanaroff–Riley I radio galaxies are commonly explained by the one-zone leptonic synchrotron self-Compton (SSC) model. Spectral modeling of correlated multiwavelength data gives the comoving magnetic field strength, the bulk outflow Lorentz factor, and the emission region size. Assuming the validity of the SSC model, the Hillas condition shows that only in rare cases such sources accelerate protons to much above 1019 eV, so ≳ 1020 eV ultra-high-energy cosmic rays (UHECRs) are likely to be heavy ions if powered by this type of radio-loud active galactic nuclei (AGNs). Survival of nuclei is shown to be possible in TeV BL Lacs and misaligned counterparts with weak photohadronic emissions. Another signature of hadronic production is intergalactic UHECR-induced cascade emission, which is an alternative explanation of the TeV spectra of some extreme non-variable blazars such as 1ES 0229+200 or 1ES 1101−232. We study this kind of cascade signal, taking into account effects of the structured extragalactic magnetic fields in which the sources should be embedded. We demonstrate the importance of cosmic-ray deflections on the γ-ray flux, and show that required absolute cosmic-ray luminosities are larger than the average UHECR luminosity inferred from UHECR observations and can even be comparable to the Eddington luminosity of supermassive black holes. Future TeV γ-ray observations using the Cerenkov Telescope Array and the High Altitude Water Cerenkov detector array can test for UHECR acceleration by observing >25 TeV photons from relatively low redshift sources such as 1ES 0229+200, and ≳TeV photons from more distant radio-loud AGNs.