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.