We make use of the results of a one-ion model of McKenzie et al. (1997
) to obtain the critical solution describing the acceleration of a two
-ion solar wind. The model includes preferential heating of the heavy
ion species and the temperature anisotropy expected if the heating is
predominantly due to ion-cyclotron damping. The relationship of the mo
del to the picture emerging from UVCS/SOHO observations is discussed.