确定Cosmic Ray表面探测器能标和μ子数的模型无关方法
A Model-Independent Method of Determining Energy Scale and Muon Number in Cosmic Ray Surface Detectors
摘要：
表面探测器阵列通过探测由初级宇宙射线引起的广延空气簇射（EAS）的次级粒子通量来测量高能宇宙射线的光谱和成分。电磁粒子和μ子是对地面探测器信号的主要贡献。在本文中，我们表明，地面信号存款的EAS可以描述的只有很少的参数：一次能量E，天顶角θ，距离的簇射最大X_max到地面，和μ子通量归一化N_mu。这组物理参数足以预测地面平均粒子通量，精度约为10%。我们表明，这是有效的强子空气淋浴，使用两个标准的强子相互作用模型在宇宙射线物理学，QGSJetII和Sibyll，并从质子到铁的原色。在此基础上，提出了一种新的地面阵列实验能量标度标定方法，该方法克服了目前地面阵列实验能量标度标定中固有的模型依赖性。此外，该方法产生EAS中μ子的平均数量的测量。然后，结合荧光探测器的X_max测量值，对宇宙线空气簇射的N_mu分布进行分析，从而对宇宙线组成和强子相互作用模型提出约束。
英文摘要：
Surface detector arrays are designed to measure the spectrum and composition of high-energy cosmic rays by detecting the secondary particle flux of the Extensive Air Showers (EAS) induced by the primary cosmic rays. Electromagnetic particles and muons constitute the dominant contribution to the ground detector signals. In this paper, we show that the ground signal deposit of an EAS can be described in terms of only very few parameters: the primary energy E, the zenith angle theta, the distance of the shower maximum X_max to the ground, and a muon flux normalization N_mu. This set of physical parameters is sufficient to predict the average particle fluxes at ground level to around 10% accuracy. We show that this is valid for hadronic air showers, using the two standard hadronic interaction models used in cosmic ray physics, QGSJetII and Sibyll, and for primaries from protons to iron. Based on this model, a new approach to calibrating the energy scale of ground array experiments is developed, which factors out the model dependence inherent in such calibrations up to now. Additionally, the method yields a measurement of the average number of muons in EAS. The measured distribution of N_mu of cosmic ray air showers can then be analysed, in conjunction with measurements of X_max from fluorescence detectors, to put constraints on the cosmic ray composition and hadronic interaction models.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
