Numerical 3-D time-dependent MHD model of the solar wind

A fully three-dimensional, time-dependent MHD model of the solar corona and the solar wind is developed. The proposed model is an upgrading of the steady-state model (Usmanov, 1993a,b). A numerical self-consistent solution for 3-D MHD equations is constructed for the region between the solar photosphere and 1.5 AU. The unique features of the proposed model are: (i) uniform coverage and self-consistent treatment of the regions of subsonic/sub-Alfvénic and supersonic/super-Alfvénic flows, (ii) as a background for transients, a steady-state solution for the ambient solar wind is used. The parameters of the initial pulses are prescribed in terms of the near-Sun shock velocities (as inferred from the metric Type II radio burst observations) relative to the preshock steady-state flow parameters.