Abstract
The collision-dominated two-fluid plasma models of the solar wind are shown to become collisionless and subject to microinstabilities at a few solar radii. Assuming that once the plasma is unstable it stays close to marginal stability models of the solar wind are constructed including waves and proton heating. The resulting models have higher velocities and proton temperatures than the collision dominated two fluid models.
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References
Feldman, W. C., Asbridge, J. R., Bame, S. J., and Gosling, J. T.: 1977, in O. R. White (ed.), The Solar Output and its Variation, Colorado Associated University Press.
Forslund, D. W.: 1970, J. Geophys. Res. 75, 17.
Hartle, R. E. and Sturrock, P. A.: 1968, Astrophys. J. 151, 1155.
Hollweg, J. V.: 1973, Astrophys. J. 181, 547.
Jacques, S. A.: 1977, Astrophys. J. 215, 942.
Singer, C. E.: 1977, J. Geophys. Res. 82, 2686.
Singer, C. E. and Roxburgh, I. W.: 1977, J. Geophys. Res. 82, 2677.
Wolff, C. L., Brandt, J. C., and Southwick, R. G.: 1971, Astrophys. J. 165, 181.
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Proceedings of the 14th ESLAB Symposium on Physics of Solar Variations, 16–19 September 1980, Scheveningen, The Netherlands.
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Rowse, D.P., Roxburgh, I.W. & Schwartz, S.J. Microinstabilities and models of the solar wind. Sol Phys 74, 179–185 (1981). https://doi.org/10.1007/BF00151288
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DOI: https://doi.org/10.1007/BF00151288