\begin{document}$ Z>2 $\end{document} data yield a medium-energy diffusion slope \begin{document}$ \delta_{2}\sim\left(0.42, 0.48\right) $\end{document} and a high-energy slope \begin{document}$ \delta_{3}\sim\left(0.22, 0.34\right) $\end{document}. The \begin{document}$ Z\leq2 $\end{document} species place a looser constraint on \begin{document}$ \delta_{2}\sim\left(0.38, 0.47\right) $\end{document} but a tighter constraint on \begin{document}$ \delta_{3}\sim\left(0.21, 0.30\right) $\end{document}. The overlaps imply that heavy and light particles can provide compatible results at medium to high energies. Moreover, both the light and heavy nuclei indicate a consistent diffusion slope variation \begin{document}$ \Delta\delta_{H} $\end{document} at \begin{document}$ 200\sim300 $\end{document} GV. At low energies, significant disagreements exist between heavy and light elements. The boron-to-carbon ratio requires a much larger diffusion slope shift \begin{document}$ \Delta\delta_{L} $\end{document} at approximately 4 GV or a stronger Alfvén velocity \begin{document}$ v_{A} $\end{document} than the low-mass data. This indicates that the heavy and light particles may suffer different low-energy transport behaviors in the galaxy. However, a better understanding of 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, a more accurate estimation of the galaxy halo size, and a more robust description of solar modulation during the reversal period of the heliospheric magnetic field."> Testing the consistency of propagation between light and heavy cosmic ray nuclei -
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