Extreme high-energy peaked BL Lac objects (EHBLs) are an emerging class of blazars with exceptional spectral properties, e.g., enhanced emission in the hard X-ray region and a hard spectrum at very high \(\gamma \)-ray energies. Currently, no suitable model exists to explain the high-energy radiation mechanism of EHBLs. Here we apply a new model of the emission process to describe the Spectral Energy Distribution (SED) of EHBLs composed of two separate components. The internal component occurs in the jet, describes synchrotron radiation and inverse Compton (IC) scattering of ultra-relativistic electrons; the two processes produce two humps of SED. The external component occurs out of the jet and considers the interaction of the proton accelerated in the jet with the cosmic microwave background (CMB), which generates electron pairs and, in turn, a cascade spectrum due to the IC scattering of those pairs with soft photons. We reproduce the SED of eight EHBLs by finding suitable values of the parameters, meanwhile, compare the \(\gamma \)-ray flux with the sensitivity of Large High Altitude Air Shower Observatory (LHAASO) and verify if these objects will be observable with LHAASO. Furthermore, we discuss the influence of intergalactic magnetic fields (IGMFs) of strength \(5\times 10^{-18}\;\mathrm{{G}\leq B_{IG}\leq 5\times 10^{-14}\;}\mathrm{{G}}\) and the region of proton’s turbulence acceleration. Finally, we find that the model may be employed to explain the high-energy emission mechanism and predict that LHAASO may detect the high-energy data of 1ES 0347-121, 1ES 1218+304, 1ES 1959+650, 1ES 2344+514 and RGB J0710+591 in the near future.

极高能峰BL Lac物体（EHBLs）是新兴的一类具有特殊光谱特性的blazar，例如，在硬X射线区域的发射增强，并且在非常高的\（\ gamma \）下的硬光谱射线能量。目前，尚无合适的模型来解释EHBLs的高能辐射机理。在这里，我们采用一种新的发射过程模型来描述由两个单独的成分组成的EHBL的光谱能量分布（SED）。内部成分发生在射流中，描述了超相对论电子的同步辐射和康普顿逆散射。这两个过程会产生两个SED峰。外部成分出现在射流之外，并考虑了射流中加速的质子与宇宙微波本底（CMB）的相互作用，后者会生成电子对，进而由于这些对的IC散射而产生电子对，从而形成级联谱光子。通过找到合适的参数值，我们再现了八个EHBL的SED，同时比较了\（\ gamma \）-具有大型高空空气淋浴天文台（LHAASO）灵敏度的射线通量，并验证是否可以使用LHAASO观察到这些物体。此外，我们讨论了强度\（5×10 ^ {-18} \; \ mathrm {{G} \ leq B_ {IG} \ leq 5 \×10 ^ { -14）的星际磁场（IGMF）的影响} \;} \ mathrm {{G}} \）和质子湍流加速区域。最后，我们发现该模型可用于解释高能排放机制，并预测LHAASO可能检测到1ES 0347-121、1ES 1218 + 304、1ES 1959 + 650、1ES 2344 + 514和RGB J0710 + 591在不久的将来。