An MHD Solar Wind Model with Turbulence Transport

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https://adsabs.harvard.edu/full/2009ASPC..406..160U

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http://hdl.handle.net/11603/30757

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UMBC Goddard Planetary Heliophysics Institute (GPHI)

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https://orcid.org/0000-0002-5317-988X

Date

2009

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conference papers and proceedings
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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. https://adsabs.harvard.edu/full/2009ASPC..406..160U

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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.
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Abstract

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.