Simple models are described which investigate the combined effects on solar wind He++ of resonant and nonresonant acceleration by left-hand transverse waves. The principal points are the following. (1) For a wide range of parameters (&ngr;&agr;--&ngr;&rgr;) at 1 AU is close to the effective phase speed of the left-hand waves. (2) The most important factor in determining &ngr;&agr;/&ngr;&rgr; at 1 AU is close is whether the high-frequency left-hand waves are predominantly outward propagating, inward propagating, inward propagating, or a mix of both. The resonant acceleration may be more important than the effects of heating or stream-stream interactions. (3) Reasonable values of &ngr;&agr;/&ngr;&rgr; at the sun (and of na/n&rgr; at 1 AU) are obtained for a power law index &agr;?1.5 in the wave power spectrum if the effective phase speed of the resonant waves near the sun is not small in comparison to the Alfv¿n speed there. This requires a substantial level of high-frequency power in outward going waves at the sun, which cannot come from heat-conduction-driven instabilities. (4) The present models do not allow one to decide whether the coronal He++ abundance is greater or less than that at 1 AU. (5) Some of the models show a positive correlation between n&agr;/n&rgr; and &ngr;&rgr; at 1 AU, roughly as has been observed. (6) The models suggest that variations in n&agr;/n&rgr; at 1 AU can result from variations in the wave properties near the sun and not neccessarily from variations in the coronal abundance. (7) Some models indicate that (&ngr;&agr;/&ngr;&rgr;) may decrease with increasing r in the vicinity of 1 AU. (8) The resonant acceleration is more efficient than Coulomb friction in the sense that it does not exhibit a runaway effect. (9) Observations of minor species may be used to deduce wave properties and plasma processes in the solar wind.