1995/05/01 by Akira Kageyama, Tetsuya Sato, the Complexity Simulation Groupa) · 8 citations
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Geomagnetism and Paleomagnetism Studies #Solar and Space Plasma Dynamics #Magnetic and Electromagnetic Effects #Physics #Dynamo theory #Dynamo #Magnetohydrodynamic drive #Convection #Kinetic energy #Electrical resistivity and conductivity #Magnetic field #Magnetic energy #Magnetohydrodynamics #Mechanics #Solar dynamo #Classical mechanics #Condensed matter physics #Magnetization
paper · doi:10.1063/1.871485
openalex publication_date 1995/05/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/06/26
A computer simulation of a magnetohydrodynamic dynamo in a rapidly rotating spherical shell is performed. Extensive parameter runs are carried out changing electrical resistivity. When resistivity is sufficiently small, total magnetic energy can grow more than ten times larger than total kinetic energy of convection motion which is driven by an unlimited external energy source. When resistivity is relatively large and magnetic energy is comparable or smaller than kinetic energy, the convection motion maintains its well-organized structure. However, when resistivity is small and magnetic energy becomes larger than kinetic energy, the well-organized convection motion is highly irregular. The magnetic field is organized in two ways. One is the concentration of component parallel to the rotation axis and the other is the concentration of perpendicular component. The parallel component tends to be confined inside anticyclonic columnar convection cells, while the perpendicular component is confined outside convection cells.