Turbulent Diffusion of the Radial Magnetic Field at the Solar Surface.

Details Turbulent Diffusion of the Radial Magnetic Field at the Solar Surface. Turbulent Diffusion of the Radial Magnetic Field at the Solar Surface.

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh41a..06g&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH41A-06

Physics

2159 Plasma Waves And Turbulence, 7524 Magnetic Fields, 7529 Photosphere, 7843 Numerical Simulation Studies, 7859 Transport Processes

Scientific paper

We discuss the physics of the diffusion of passive additives embedded within a turbulent fluid. Simple numerical experiments are performed. These are designed to determine the relevant diffusion equation associated with the additive's motions. Our results are compared with analytic theory. We find that for the case in which the fluid is incompressible (zero divergence) and spatially inhomogeneous, the standard diffusion equation describes the spatial distribution of passive additives. However, for the case in which the turbulent fluid has a nonzero divergence, a different "diffusion" equation is needed to describe their spatial distribution. For this case, the equation derived by Parker ("Interplanetary Dynamical Processes", 1963) and more recently by Fisk and Schwadron (Astrophys. J., 560, 425, 2001) is applicable. Implications of these results will be discussed, particularly how they relate to the transport of the radial magnetic field at the solar surface due to photospheric motions.

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