Abstract
We present a new approach to the theory of magnetohydrodynamic equilibria with anisotropic pressure, magnetic shear and translational/rotational invariance. This approach involves combining two existing formalisms in order to eliminate their individual weaknesses. The theoretical aspects of the method are explored in detail along with numerical solutions which make use of the method. Eventually, this method could be applied to model various plasma systems, such as planetary magnetospheres.
Highlights
Magnetohydrodynamic (MHD) equilibria can be used to model a wide variety of physical processes, with applications varying from astrophysical systems such as magnetospheres and the sun, to laboratory plasmas such as those confined within tokamaks and stellarators
There is a good motiv ation to consider switching between these formalisms, which we call the combined approach: we can ensure a sensible definition of the pressure in terms of the total magnetic field strength, whilst avoiding the implicit coupling problem, shear field contradictions and the difficulties involving scale factors
We suggest that the combined formalism should be used as the new standard method of computing anisotropic pressure MHD equilibria
Summary
Magnetohydrodynamic (MHD) equilibria can be used to model a wide variety of physical processes, with applications varying from astrophysical systems such as magnetospheres and the sun, to laboratory plasmas such as those confined within tokamaks and stellarators. There is a good motiv ation to consider switching between these formalisms, which we call the combined approach: we can ensure a sensible definition of the pressure in terms of the total magnetic field strength, whilst avoiding the implicit coupling problem, shear field contradictions and the difficulties involving scale factors. For these reasons, we suggest that the combined formalism should be used as the new standard method of computing anisotropic pressure MHD equilibria.
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