Boosting the Magnetic Field of a Toroidal Conductive Fluid by a Poloidal Flow

抄録

Researchers have struggled to understand the mechanism underlying the formation of celestial magnetic fields. Currently, the generation of axisymmetric and poloidal magnetic fields can be solved by complex convection arguments. There are also simple convection claims, but they all assert that magnetic field generation is by simple convection by treating it as an approximation or nonlinear process. This paper addresses a truly simple axisymmetric poloidal convection and magnetic field. To calculate the electrical components, this paper introduces a theory that separates the vector potential into inductance and current in a relational formula. The reason is to consider the mutual influence between distant circuits in terms of mutual inductance. Then, the change in current is calculated from the change in inductance. It is solved as an eigenvalue problem. By this method, it is proven that a simple axisymmetric poloidal magnetic field can be generated from axisymmetric poloidal convection. Another reason is the nature of mutual inductance and Lenz’s law, which reflects the effect of current changes on other electrical circuits. This is intended to eliminate the concern that magnetic field growth will be impaired by magnetic field freezing. These are novel concepts, and we believe that these findings will contribute to further elucidating the formation mechanism of celestial magnetic fields and plasma reactor research. However, regarding the stability of the magnetic field, the behavior of convection itself must be considered, but since this topic is not included in this paper, only the concept is described.