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Self-consistent magnetohydrodynamic coronal hole flows

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Abstract

Magnetic fields are thought to play a crucial role in determining the dynamics and energetics of coronal hole flows. In this paper we investigate the possibility that the large scale structure of the magnetic field and plasma within a coronal hole may be determined from the effects of plasma-magnetic field interactions. The overall state is then governed by a complex balance of inertial, pressure gravitational and magnetic forces. Integration of the highly non-linear system of differential equations, which describe the plasma-magnetic field coupling, is made possible by employing a numerical iterative technique developed by Pneuman and Kopp (1971). The method of solution is modified and extended to describe thermally conductive plasma flow in coronal holes. We consider the features of a typical converged solution, representing the distribution of velocity, temperature, density and magnetic field strength within a coronal hole.

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  1. Department of Applied Mathematics, Queen Mary College, University of London, Mile End Road, E1 4NS, London, U.K.

    Barry J. Robertson

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  1. Barry J. Robertson
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Robertson, B.J. Self-consistent magnetohydrodynamic coronal hole flows. Sol Phys 83, 63–82 (1983). https://doi.org/10.1007/BF00148243

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  • DOI: https://doi.org/10.1007/BF00148243

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