STELLAR WINDS WITH NON-WKB ALFVEN WAVES .1. WIND MODELS FOR SOLAR CORONAL CONDITIONS

We have constructed numerical models for stationary, wind-type outflow s that include treatment of the force produced by propagating Alfven w aves. We make no assumptions regarding the relative sizes of the wavel engths of such disturbances and the scale lengths that characterize th e variation of the physical properties of the expanding stellar atmosp here. Consequently, our models take into account the process of Alfven wave reflection, and provide for dynamical effects arising from the s imultaneous presence of outward and inward traveling waves in the wind . For physical conditions like those prevailing in the outer solar cor ona and wind, we find that even relatively high frequency, short wavel ength waves can suffer some reflection from the gradient in Alfven spe ed at the base of the flow. Among the consequences of the interaction between outward and inward directed perturbations in the sub-Alfvenic portion of the wind is a reduction in the magnitude of the time-averag ed wave force relative to its value in the WKB (i.e., short-wavelength ) limit. As a result, the flow velocities of our models interior to th e Alfven radius are smaller than those of corresponding WKB models. Fo r models containing very low frequency, long wavelength waves, a subst antial amount of wave reflection can also take place in the super-Alve nic portion of the wind. The resulting modifications to the spatial de pendences of the wave magnetic and velocity amplitudes can lead to a w ave force whose magnitude at large distances exceeds that of an equiva lent WKB solution.