Testing the consistency of proapgation between light and heavy cosmic
  ray nuclei
  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 high-energy diffusion
slope $\delta_{2}\sim$ (0.37, 0.44). The $Z\leq2$ species obtain a looser
constraint on $\delta_{2}\sim$ (0.34, 0.44). The overlap infers the heavy and
light particles can give compatible results at high energies. Meanwhile, at low
energies, significant disagreements exist between the heavy and light elements.
The B/C ratio requires a much larger diffusion slope variation
$\delta_{2}$-$\delta_{1}$ 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 relies on more precise cross-sections, better constraints on
correlations in systematic errors of data, and more accurate description for
Solar modulation during the reversal period of HMF.
