We study the interaction between protons, multiple minor ions (O5+, He++), and a given Alfv¿n/cyclotron fluctuation spectra in the corona and the solar wind. One-dimensional hybrid simulations are performed in initially homogeneous, collisionless, magnetized plasma with waves propagating parallel to the background magnetic field. The self-consistent hybrid simulations and linear Vlasov theory are used to study the effect of the driving spectrum, ion drift velocity, and microinstabilities on the coronal plasma and solar wind heating. The simulation results provide a clear picture of wave-particle interaction and successfully explain (1) how the driving spectrum frequency range and the power law index affect the resonant heating, (2) how ion double-peak distribution is formed and how differential flows affect the resonant interaction via the change of the resonant wave dispersion relation, and (3) how local microinstabilities affect minor ion heating and constraint the values of plasma parameters observed in the solar wind.