标题： 测试轻核与重宇宙射线核之间的传播一致性 显示英文标题

标题： Testing the consistency of proapgation between light and heavy cosmic ray nuclei

摘要： 宇宙射线物理中的一个基本问题是解释宇宙射线加速和传播机制的性质。 得益于最近空间实验测得的精确宇宙射线数据，我们能够更全面和可靠地研究宇宙射线加速和传播模型。 在本文中，我们将PAMELA、AMS02、ACE-CRIS和Voyager-1测量的次级与初级比值和初级谱结合起来，以限制宇宙射线源和传输参数。 研究表明，$Z>2$数据得出中能区扩散斜率$\delta_{2}\sim\left(0.42, 0.48\right)$和高能区斜率$\delta_{3}\sim\left(0.22, 0.34\right)$。 $Z\leq2$种类对$\delta_{2}\sim\left(0.38, 0.47\right)$的约束较松，但对$\delta_{3}\sim\left(0.21, 0.30\right)$的约束更紧。 重叠结果表明，重粒子和轻粒子在中高能区可以给出相容的结果。 此外，轻核和重核均显示出在约$200\sim300$~GV 附近一致的扩散斜率变化$\Delta\delta_{H}$。 在低能区，重元素和轻元素之间存在显著的不一致。 B/C 比值需要在 4 GV 左右有更大的扩散斜率变化$\Delta\delta_{L}$，或者比低质量数据更强的\textit{阿尔芬$\acute{e}$速度} $v_{A}$ 。 这表明重粒子和轻粒子在银河系中可能经历不同的低能传输行为。 然而，要更好地理解重宇宙射线和轻宇宙射线之间的一致性/不一致性，需要更精确的截面数据，对数据系统误差相关性的更好约束，对银河晕大小更准确的估计，以及对太阳调制在地磁场反转期间更稳健的描述。 显示英文摘要

摘要： One of the fundamental issues in cosmic ray physics is to explain the nature of cosmic ray acceleration and propagation mechanisms. Thanks to the precise cosmic ray data measured by recent space experiments, we are able to investigate the cosmic ray acceleration and propagation models more comprehensively and reliably. In this paper, we combine the secondary-to-primary ratios and the primary spectra measured by PAMELA, AMS02, ACE-CRIS and Voyager-1 to constrain the cosmic ray source and transport parameters. The study shows that the $Z>2$ data yield a medium-energy diffusion slope $\delta_{2}\sim\left(0.42, 0.48\right)$ and a high-energy slope $\delta_{3}\sim\left(0.22, 0.34\right)$. The $Z\leq2$ species obtain a looser constraint on $\delta_{2}\sim\left(0.38, 0.47\right)$, but a tighter constraint on $\delta_{3}\sim\left(0.21, 0.30\right)$. The overlaps infer that the heavy and light particles can give compatible results at medium to high energies. Besides, both the light and heavy nuclei indicate a consistent diffusion slope variation $\Delta\delta_{H}$ around $200\sim300$~GV. At low energies, significant disagreements exist between the heavy and light elements. The B/C ratio requires a much larger diffusion slope shift $\Delta\delta_{L}$ around 4 GV or a stronger \textit{Alfv$\acute{e}$n velocity} $v_{A}$ than the low-mass data. This indicates that the heavy and light particles may suffer different low-energy transport behaviors in Galaxy. However, better understanding on the consistency/inconsistency between the heavy and light cosmic rays relies on more precise cross-sections, better constraints on correlations in systematic errors of data, more accurate estimation on Galaxy halo size and more robust description for Solar modulation during the reversal period of HMF.