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(Te) and proton(Tp) temperatures and solar wind speed(V) at 1 AU. As a result, we obtained physical quantities of solar wind as follows: Te is 7.4 X 10.5 K and density(n) is 1.7 X 107 cm-3 in the corona. At 1 AU Te is 2.1 X 105 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.

• Y. D. PARK(Korea Astronomy Observatory, Department of Astronomy & Space Science, Kyunghee University/ Big Bear Solar Observatory, NJIT)
• K.-S. CHO(Korea Astronomy Observatory, Department of Astronomy & Space Science, Kyunghee University)
• Y.-J. MOON(Korea Astronomy Observatory, Department of Astronomy & Space Science, Kyunghee University)
• K.-S. KIM(Department of Astronomy & Space Science, Kyunghee University)
• S.-J. KIM(Korea Astronomy Observatory, Department of Astronomy & Space Science, Kyunghee University/Department of Astronomy & Space Science, Kyunghee University) Corresponding Author