  The secondary-to-primary ratios are unique tools to investigate cosmic ray
propagation mechanisms. In this work, we use the latest data of
deuteron-to-helium~4 ratio and helium~3-to-helium~4 ratio measured by PAMELA
combined with other Z$\leq$2 primary fluxes measured by PAMELA and Voyager-1,
to constrain the cosmic ray acceleration and propagation models. The analysis
is performed by interfacing statistical tools with the GALPROP propagation
package. To better fit both the modulated and unmodulated low energy cosmic ray
data, we find that a time-, charge- and rigidity-dependent solar modulation
model is better than the force-field approximation. Among all the studied
cosmic ray propagation models, the diffusion-reacceleration-convection model is
strongly supported by the derived Bayesian evidence. The robustness of the
estimated diffusion slope $\delta$ is cross-checked by another low-mass
secondary-to-primary ratio, i.e. the antiproton-to-proton ratio. It is shown
that the diffusion-reacceleration-convection model can reconcile well with the
high energy antiproton-to-proton ratio. This indicates that the estimated value
of $\delta$ is reliable. The well constraint $\delta$ from the `best' model is
found to be close to 1/3, inferring a Kolmogorov-type interstellar magnetic
turbulence.
