Galactic, Astrophysical and Planetary Dynamos

Dear Colleagues,

Large-scale magnetic fields are observed surrounding galaxies, stars, and planets and are thus universal phenomena. These magnetic fields are believed to be due to magnetohydrodynamics (MHD) processes in the energetic, turbulent magnetofluids that lie within these objects. One important characteristic observed is the dominance of a quasi-steady dipole component. It has long been realized that MHD dynamos must exist to create large-scale, i.e., dipole, magnetic fields. A full understanding of the origin and evolution of these large-scale magnetic fields will result in a solution to the “dynamo problem”. Historical approaches to studying these phenomena, such as kinematic dynamo theory and mean-field electrodynamics, have, in general, proven unsatisfactory. For this Special Issue of Fluids, we solicit papers presenting modern approaches to understanding galactic, astrophysical, and planetary dynamos. The focus of these papers may include MHD turbulence, inertial wave effects, mechanisms for forcing and dipole alignment, creation of plasma jets and mass ejections, and other related topics. The MHD dynamos studied may range from those in planets and stars to those in active galactic nuclei, in the galaxy as a whole, and in galaxy clusters, i.e., both non-relativistic and relativistic physical phenomena. Methods of study can include theoretical analysis, statistical mechanics, numerical simulation, and astronomical observation.

Prof. Dr. John Shebalin
Guest Editor

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