从$X_{\mathrm{max}}$分布尾部测量超高能质子氦比的下限
Lower limit on the ultra-high-energy proton-to-helium ratio from the measurements of the tail of $X_{\mathrm{max}}$ distribution
摘要：
有多种技术可以确定超高能宇宙射线的化学成分。虽然大多数方法主要对平均原子质量敏感，但区分两种最轻的元素：质子和氦是具有挑战性的。本文利用簇射极大值$X_{\mathrm{max}}$的深度分布的尾部估计了能量范围为$10^{18.0} \mbox{eV}$至$10^{19.3} \mbox{eV}$的质子氦比。利用皮埃尔俄歇天文台和望远镜阵列实验测量的指数衰变标度$Λ$，导出了相应于$10^{18.0} < E < 10^{18.5}$ eV和$10^{18.3} < E < 10^{19.3}$ eV的质子氦比$\mathrm{p}/\mathrm{He} > 7.3 $和$\mathrm{p}/\mathrm{He} > 0.43 $的68\\，CL约束.结果表明，对于较重元素的混合，该结果是保守的。我们评估的强子相互作用模型的不确定性的影响。讨论了对宇宙射线起源的天体物理模型和未来对撞机安全性的影响。
英文摘要：
There are multiple techniques to determine the chemical composition of the ultra-high-energy cosmic rays. While most of the methods are primarily sensitive to the average atomic mass, it is challenging to discriminate between the two lightest elements: proton and helium. In this paper, the proton-to-helium ratio in the energy range $10^{18.0} \mbox{eV}$ to $10^{19.3} \mbox{eV}$ is estimated using the tail of the distribution of the depth of the shower maximum $X_{\mathrm{max}}$. Using the exponential decay scale $Λ$ measured by the Pierre Auger Observatory and the Telescope Array experiment we derive the 68\%\,CL constraints on the proton-to-helium ratio $\mathrm{p}/\mathrm{He} > 7.3 $ and $\mathrm{p}/\mathrm{He} > 0.43 $ for $10^{18.0} < E < 10^{18.5}$ eV and $10^{18.3} < E < 10^{19.3}$ eV correspondingly. It is shown that the result is conservative with respect to the admixture of heavier elements. We evaluate the impact of the hadronic interaction model uncertainty. The implications for the astrophysical models of the origin of cosmic rays and the safety of the future colliders are discussed.
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。
