A fully three-dimensional, steady-state global model of the solar coro
na and the solar wind is developed. A numerical, self-consistent solut
ion for 3-D MHD equations is constructed for the region between the so
lar photosphere and the Earth's orbit. Boundary conditions are provide
d by the solar magnetic field observations. A steady-state solution is
sought as a temporal relaxation to the dynamic equilibrium in the reg
ion of transonic flow near the Sun and then traced to the orbit of the
Earth in supersonic flow region. The unique features of the proposed
model are: (a) uniform coverage and self-consistent treatment of the r
egions of subsonic/sub-Alfvenic and supersonic/super-Alfvenic flows, (
b) inferring the global structure of the interplanetary medium between
the solar photosphere and 1 AU based on large-scale solar magnetic fi
eld data. As an experimental test for the proposed technique, photosph
eric magnetic field data for CR 1682 are used to prescribe boundary co
ndition near the Sun and results of a simulation are compared with spa
cecraft measurements at 1 AU. The comparison demonstrates a qualitativ
e agreement between computed and observed parameters. While the differ
ence in densities is still significant, the 3-D model better reproduce
s variations of the solar wind velocity than does the 2-D model presen
ted earlier (Usmanov, 1993).