MHD modeling of the solar wind with turbulence transport and heating
A. V. Usmanov 1,2, W. M. Matthaeus 1, B. Breech M. 2 and M. L. Goldstein 2
1 Department of Physics and Astronomy and Bartol Research Institute, University of Delaware, Newark, DE 19716
2 Code 673, NASA Goddard Space Flight Center, Greenbelt, MD 2077
We have developed a magnetohydrodynamic model that describes the global axisymmetric steady-state structure of the solar wind near solar minimum
with account for transport of small scale turbulence associated heating.
The Reynolds-averaged mass, momentum, induction, and energy equations for the large-scale solar wind flow are solved simultaneously with the
turbulence transport equations in the region from 0.3 to 100 AU. The
large-scale equations include subgrid-scale terms due to turbulence and the
turbulence (small-scale) equations describe the effects of transport and
(phenomenologically) dissipation of the MHD turbulence based on a few
statistical parameters (turbulence energy, normalized cross-helicity, and
correlation scale). The coupled set of equations is integrated numerically for a source dipole field on the Sun by a time-relaxation method in the corotating frame of reference. We present results on the plasma, magnetic field, and turbulence distributions throughout the heliosphere and on the role of the turbulence in the large-scale structure and temperature distribution in the solar wind.