Particle accelerators abound in space plasmas, saturating the cosmos with fully stripped nuclei and gamma rays, with energies surpassing the capabilities of human-made accelerators by orders of magnitude. Upon reaching Earth’s atmosphere, these particles trigger extensive air showers (EASs), generating millions of secondary cosmic rays of lower energies. Free electrons from EASs developing in the atmosphere are seeds for atmospheric electron accelerators. Strong atmospheric electric fields (AEFs) evolving during thunderstorms act as accelerators, amplifying the intensity of electrons many times, significantly enlarging the EAS size (number of electrons). Thus, the energy of the primary cosmic ray recovered by EAS size can be significantly overestimated. Recently discovered by high-altitude EAS arrays, PeVatron candidates (ultra–high-energy (UHE) astrophysical gamma-ray sources) must be carefully examined according to the atmospheric conditions during EAS detection. Large High Altitude Air Shower Observatory and High-Altitude Water Cherenkov Observatory arrays are located in regions of frequent thunderstorms, and an AEF’s strength can reach and surpass the critical strength to start relativistic runaway electron avalanches. A few registered UHE gamma rays from stellar sources can be registered at just this time when the AEF highly enhances the EAS size. Thunderstorm ground enhancements are copiously registered at mountain peaks of Eastern Europe, Germany, and Armenia, with energies well above the threshold energy of EAS array scintillators. Thus, the overestimation of the energy of primary particles is not an exotic process but a consequence of already well-established physical phenomena. Consequently, a report on each registered UHE gamma ray should include the recorded time and corresponding weather conditions.

中文翻译：

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雷暴期间天体物理伽马射线能量的高估：银河和大气加速器的协同作用


粒子加速器在太空等离子体中比比皆是，用完全剥离的原子核和伽马射线使宇宙饱和，其能量超过了人造加速器的能力几个数量级。到达地球大气层后，这些粒子会触发大范围风雨 （EAS），产生数百万条较低能量的次级宇宙射线。在大气中发育的 EAS 产生的自由电子是大气电子加速器的种子。在雷暴期间演化的强大气电场 （AEF） 充当加速器，将电子的强度放大数倍，从而显着扩大 EAS 的大小（电子数）。因此，由 EAS 大小恢复的初级宇宙射线的能量可能被大大高估。最近由高空 EAS 阵列发现的 PeVatron 候选者（超高能 （UHE） 天体物理伽马射线源）必须在 EAS 探测期间根据大气条件仔细检查。大型高空气淋天文台和高空水切伦科夫天文台阵列位于雷暴频繁的区域，AEF 的强度可以达到并超过引发相对论失控电子雪崩的临界强度。当 AEF 高度增强 EAS 大小时，可以记录一些来自恒星源的 UHE 伽马射线。东欧、德国和亚美尼亚的山峰上大量记录了雷暴地面增强，其能量远高于 EAS 阵列闪烁体的阈值能量。因此，高估初级粒子的能量并不是一个奇特的过程，而是已经确立的物理现象的结果。 因此，关于每条已记录的 UHE 伽马射线的报告应包括记录的时间和相应的天气状况。