An MHD Solar Wind Model with Turbulence Transport





Citation of Original Publication

Usmanov, A. V., et al. "An MHD Solar Wind Model with Turbulence Transport." Numerical Modeling of Space Plasma Flows: ASTRONUM-2008 ASP Conference Series, Vol. 406, proceedings of the conference held 8-13 June, 2008 at The Westin Hotel, St. John, U.S. Virgin Islands.


This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
Public Domain Mark 1.0



We present initial results from an axisymmetric steady-state solar wind model that describes properties of the large-scale solar wind, interplanetary magnetic field, and turbulence throughout the heliosphere from 0.3 AU to 100 AU. The model is based on numerical solutions of large-scale Reynolds-averaged magnetohydrodynamic (MHD) equations coupled with a set of small-scale transport equations for the turbulence energy, normalized cross-helicity, and correlation scale. The combined set of the time-dependent equations is solved in the frame of reference corotating with the Sun by a time-relaxation method. We use the model to study the global solar wind structure and the distribution of turbulence throughout the heliosphere.