THE GLOBAL STRUCTURE OF THE SOLAR-WIND IN JUNE 1991

A numerical simulation of the global solar wind structure for Carringt on rotation 1843 (31 May-28 June, 1991) is performed based on a fully three-dimensional, steady-state MHD model of the solar wind (Usmanov, 1993b). A self-consistent solution for 3-D MHD equations is constructe d for the spherical shell extending from the solar photosphere up to 1 0 AU. Solar magnetic field observations are used to prescribe boundary conditions. The computed distribution of the magnetic held is compare d with coronal hole observations and with the IMF measurements made by IMP-8 spacecraft at the Earth's orbit.