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The secondary-to-primary ratios are unique tools to investigate cosmic raypropagation mechanisms. In this work, we use the latest data ofdeuteron-to-helium~4 ratio and helium~3-to-helium~4 ratio measured by PAMELAcombined with other Z$\leq$2 primary fluxes measured by PAMELA and Voyager-1,to constrain the cosmic ray acceleration and propagation models. The analysisis performed by interfacing statistical tools with the GALPROP propagationpackage. To better fit both the modulated and unmodulated low energy cosmic raydata, we find that a time-, charge- and rigidity-dependent solar modulationmodel is better than the force-field approximation. Among all the studiedcosmic ray propagation models, the diffusion-reacceleration-convection model isstrongly supported by the derived Bayesian evidence. The robustness of theestimated diffusion slope $\delta$ is cross-checked by another low-masssecondary-to-primary ratio, i.e. the antiproton-to-proton ratio. It is shownthat the diffusion-reacceleration-convection model can reconcile well with thehigh energy antiproton-to-proton ratio. This indicates that the estimated valueof $\delta$ is reliable. The well constraint $\delta$ from the `best' model isfound to be close to 1/3, inferring a Kolmogorov-type interstellar magneticturbulence.

Revisit cosmic ray propagation by using $^{1}$H, $^{2}$H, $^{3}$He and $^{4}$He