A. V. Usmanov, M. L. Goldstein, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
A
three-dimensional magnetohydrodynamic model is used to simulate the global
structure of the solar corona and solar wind in the spherical shell between
the coronal base and 100 AU. The model accounts for the effects of Alfven
wave acceleration near the Sun and for the interaction of solar wind protons
with interstellar neutral hydrogen in the outer heliosphere. We use the
time-relaxation method to construct a steady-state solution of
time-dependent equations in the inner computation region (1-20 solar radii)
and a direct integration along radius of steady-state equations outside 20
solar radii. The relaxation code is an implementation of the spatially
third-order, semi-discrete Central Weighted Essentially Non-Oscillatory
(CWENO) numerical scheme of Kurganov and Levy [2000]. We present simulation
results for the solar conditions typical of solar minimum and other phases
of the solar cycle.