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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.

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Authors and Affiliations

  1. Dept. of Physics, Boston College, 02167, Chestnut Hill, Mass., U.S.A.

    M. S. Gussenhoven & R. L. Carovillano

Authors
  1. M. S. Gussenhoven
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  2. R. L. Carovillano
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Gussenhoven, M.S., Carovillano, R.L. Restrictions on radial magnetic field and flow solutions for the solar wind. Sol Phys 29, 233–241 (1973). https://doi.org/10.1007/BF00153451

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  • DOI: https://doi.org/10.1007/BF00153451

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