3-D simulation of turbulent cyclonic magneto-convection

Details 3-D simulation of turbulent cyclonic magneto-convection 3-D simulation of turbulent cyclonic magneto-convection

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...232..277b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 232, no. 1, June 1990, p. 277-291.

Astronomy and Astrophysics

Astrophysics

84

Magnetic Diffusion, Magnetohydrodynamic Turbulence, Rayleigh-Benard Convection, Solar Magnetic Field, Three Dimensional Models, Compressible Flow, Magnetic Field Configurations, Magnetohydrodynamic Waves

Scientific paper

Results are presented of a simulation of turbulent three-dimensional magnetic convection under the influence of rotation in a fluid layer whose depth is about 1 pressure-scale hight. The approach is similar to that of Meneguzzi and Pouquet (1989), except for the assumptions that the fluid is a compressible conducting gas and there is a vanishing horizontal magnetic field at the boundaries. The results demonstrate that topological effects may be of great importance for MHD convection. It is shown that, as a consequence of topological effects, anisotropies of the alpha-effect can play a dominant role. In particular, the sign of alpha(V) can be opposite to that expected from a first-order smoothing approach.

Affiliated with

Also associated with

No associations

Rating

3-D simulation of turbulent cyclonic magneto-convection 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 3-D simulation of turbulent cyclonic magneto-convection, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and 3-D simulation of turbulent cyclonic magneto-convection will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-980750