A MHD model of 2-D structure of solar wind and magnetic field output on source surface

A MHD model is used for exploration of 2-D structure of the solar plasma outputs on the source surface (2.5 R). In this model the observational data for Kcorona brightness and the photospheric magnetic field are as inputs of MHD equations which are closed by a statistical result. Prelimilary results are that (1) 2-D distributions of velocity, temperature and mass flux outputs on the source surface are structural and in which the magnetic field plays a controlling role. (2) Comparisons between the theoretic and observational results indicate that MHD model could provide an useful description of the 2-D structure of solar wind plasma outputs near the sun and the source surface could be considered as the "source" of the interplanetary solar wind.