Using a
three-dimensional MHD model, we simulate the global steady-state structure
of the solar corona and solar wind for a dipole magnetic field on the Sun
inclined by 30 degrees to the solar rotation axis. This represents the solar
conditions typical for a declining phase of solar cycle. Our computational
domain extends from the coronal base out to 100 AU and
accounts for the population of interstellar neutral hydrogen and its
interaction with solar wind protons within the heliosphere. We will present
simulation results on the formation of corotating interaction regions and
the heliospheric current sheet, their evolution with heliocentric distance,
and the effects of pickup protons in this evolution.