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Using linear Vlasov theory of plasma waves and quasi-linear theory ofresonant wave-particle interaction, the dispersion relations and theelectromagnetic field fluctuations of fast and Alfven waves are studied for alow-beta multi-ion plasma in the inner corona. Their probable roles in heatingand accelerating the solar wind via Landau and cyclotron resonances arequantified. We assume that (1) low-frequency Alfven and fast waves have thesame spectral shape and the same amplitude of power spectral density; (2) thesewaves eventually reach ion cyclotron frequencies due to a turbulence cascade;(3) kinetic wave-particle interaction powers the solar wind. The existence ofalpha particles in a dominant proton/electron plasma can trigger linear modeconversion between oblique fast-whistler and hybrid alpha-proton cyclotronwaves. The fast-cyclotron waves undergo both alpha and proton cyclotronresonances. The alpha cyclotron resonance in fast-cyclotron waves is muchstronger than that in Alfven-cyclotron waves. For alpha cyclotron resonance, anoblique fast-cyclotron wave has a larger left-handed electric fieldfluctuation, a smaller wave number, a larger local wave amplitude, and agreater energization capability than a corresponding Alfven-cyclotron wave atthe same wave propagation angle \theta, particularly at $80^\circ$ < \theta <$90^\circ$. When Alfven-cyclotron or fast-cyclotron waves are present, alphaparticles are the chief energy recipient. The transition of preferentialenergization from alpha particles to protons may be self-modulated bydifferential speed and temperature anisotropy of alpha particles via theself-consistently evolving wave-particle interaction. Therefore, fast-cyclotronwaves as a result of linear mode coupling is a potentially important mechanismfor preferential energization of minor ions in the main acceleration region ofthe solar wind.

Roles of Fast-Cyclotron and Alfven-Cyclotron Waves for the Multi-Ion Solar Wind