In this work we use the newly reported Boron-to-Carbon ratio ( B/C ) from AMS-02 and the time-dependent proton fluxes from PAMELA and AMS-02 to constrain the source and propagation parameters of cosmic rays in the Milky Way .
A linear correlation of the solar modulation parameter with solar activities is assumed to account for the time-varying cosmic ray fluxes .
A comprehensive set of propagation models , with/without reacceleration or convection , have been discussed and compared .
We find that only the models with reacceleration can self-consistently fit both the proton and B/C data .
The rigidity dependence slope of the diffusion coefficient , \delta , is found to be about 0.38 - 0.50 for the diffusion-reacceleration models .
The plain diffusion and diffusion-convection models fit the data poorly .
We compare different model predictions of the positron and antiproton fluxes with the data .
We find that the diffusion-reacceleration models over-produce low energy positrons , while non-reacceleration models give better fit to the data .
As for antiprotons , reacceleration models tend to under-predict low energy antiproton fluxes , unless a phenomenological modification of the velocity-dependence of the diffusion coefficient is applied .
Our results suggest that there could be important differences of the propagation for nuclei and leptons , in either the Milky Way or the solar heliosphere .