Restrictions on radial magnetic field and flow solutions for the solar wind
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Abstract
In Parker's original model, the solar wind is represented as a spherically symmetric hydrodynamic flow. The velocity is radially directed and decoupled from the magnetic field. The simple extension of this model to include a dependence on the polar angle, θ, is shown to be invalid for radial flow and radial magnetic field. This work demonstrates how ad hoc symmetry conditions imposed to simplify a non-linear problem can be incompatible with the basic hydromagnetic equations.
Keywords
Magnetic Field Solar Wind Original Model Polar Angle Symmetry Condition
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