AI 中文总结
该研究表明冰中无线电探测器可通过模拟簇射的横向宽度与 Askaryan 谱形状，测量 $10^{17}$eV 以上宇宙射线质量组成，其核心宽度与 $\rm X_{max}$ 高度相关。
AI 中文摘要
冰中无线电探测器最初主要通过 Askaryan 效应开发用于探测高能中微子，但近期研究表明其对撞击冰盖的宇宙射线空气簇射也具有灵敏度。使用 CORSIKA 8 模拟撞击空气簇射，我们发现冰中级联的横向宽度对原初宇宙射线的原子质量敏感。簇射核心的宽度可通过 Askaryan 无线电谱的形状获取，而振幅则编码了冰中总电荷过剩。我们证明，若将冰中接收器放置成能充分采样 Askaryan 发射图案，冰中无线电探测器可用于测量 $10^{17}$eV 以上区域的宇宙射线质量组成。我们还表明，冰中核心宽度与粒子数最大深度（$\rm X_{max}$，重建宇宙射线质量组成最常用的可观测物理量）高度相关，但并非完全相关。
英文摘要
In-ice radio detectors have been developed primarily for the detection of high-energy neutrinos via the Askaryan effect, but have recently been shown to also be sensitive to cosmic ray air showers impacting the ice sheet. Using CORSIKA 8 to simulate impacting air showers, we find that the lateral width of the in-ice cascade is sensitive to the atomic mass of the primary cosmic ray. The width of the shower core is accessible through the shape of the Askaryan radio spectrum, while the amplitude encodes the total in-ice charge excess. Using these two observables, we show that in-ice radio detectors can be used to measure cosmic ray mass composition in the region above $10^{17}$eV if the in-ice receivers are placed to adequately sample the Askaryan emission pattern. We also show that the in-ice core width is highly, but not exactly, correlated with the depth of maximum particle count ($\mathrm{X}_{\mathrm{max}}$), the most commonly used observable for reconstructing cosmic ray mass composition.
CommentsProceedings of the 11th International Workshop on Acoustic and Radio EeV Neutrino Detection Activities, ARENA 2026
