An MHD Solar Wind Model with Turbulence Transport

Details An MHD Solar Wind Model with Turbulence Transport An MHD Solar Wind Model with Turbulence Transport

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..406..160u&link_type=abstract

Numerical Modeling of Space Plasma Flows: ASTRONUM-2008 ASP Conference Series, Vol. 406, proceedings of the conference held 8-13

Astronomy and Astrophysics

Astronomy

3

Scientific paper

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.

Affiliated with

Also associated with

No associations

Rating

An MHD Solar Wind Model with Turbulence Transport does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with An MHD Solar Wind Model with Turbulence Transport, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and An MHD Solar Wind Model with Turbulence Transport will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1238469