We have developed a two fluid solar wind model from the Sun to 1 AU. Its basic equations are mass, momentum and energy conservations. In these equations, we include a wave mechanism of heating the corona and accelerating the wind. The two fluid model takes into account the power spectrum of Alfvenic wave fluctuation. Model computations have been made to fit observational constraints such as electron($T_e$) and proton($T_p$) temperatures and solar wind speed(V) at 1 AU. As a result, we obtained physical quantities of solar wind as follows: $T_e$ is $7.4{ imes}10^5$ K and density(n) is $1.7 { imes}10^7;cm^{-3}$ in the corona. At 1 AU $T_e$ is $2.1 { imes} 10^5$ K and n is $0.3 cm^{-3}$, and V is $511 km;s^{-1}$. Our model well explains the heating of protons in the corona and the acceleration of the solar wind.