Abstract
A fluid mechanical convective instability is examined under the conditions found in the solar corona. Linearized density perturbations are shown to grow as they are carried outward by the solar wind. The non-linear instability may be proposed as a cause of coronal structures in non-magnetic stars, or in regions of the solar corona with weak magnetic fields.
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References
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Cross, M.A., Blockwood, J.V. Structures in a non-magnetic solar corona. Sol Phys 38, 157–164 (1974). https://doi.org/10.1007/BF00161832
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DOI: https://doi.org/10.1007/BF00161832