A. V. Usmanov, M. L. Goldstein, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
We
compute the global three-dimensional steady-state structure of the solar
wind and interplanetary magnetic field from the base of solar corona to 100
AU and compare the simulated plasma and magnetic field parameters with
Voyager 1 and 2 measurements. Our tilted-dipole model of the solar
corona and solar wind is appropriate for solar minimum conditions and
assumes a uniform distribution of neutral hydrogen throughout the
heliosphere. The inclusion of the pickup protons causes a deceleration of
the solar wind and an increase in average plasma temperature with
heliocentric distance. The three-dimensional character of the model allows
us to study both radial and latitudinal effects. The model is consistent
with the changes in the proton temperature observed by Voyager 2 as it moves
to higher southern latitudes in the outer heliosphere.