  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.
