Abstract
Due to high temperature and more importantly a small temperature gradient with height the solar corona is not in hydrostatic equilibrium but is continuously expanding into interplanetary space. The resulting outflow of coronal plasma is known as the solar wind. Because of the very high electrical conductivity of the coronal plasma the magnetic field in the corona controls both the heat conduction and the basic outflow of material. In regions where the magnetic field lines reach high into the corona (e.g. over coronal holes) the coronal expansion is greatly enhanced.
This work was supported by the National Aeronautics and Space Administration under Contract NAS5-22993.
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Svalgaard, L. (1977). Solar Wind and Interplanetary Medium. In: Bruzek, A., Durrant, C.J. (eds) Illustrated Glossary for Solar and Solar-Terrestrial Physics. Astrophysics and Space Science Library, vol 69. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-1245-4_13
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DOI: https://doi.org/10.1007/978-94-010-1245-4_13
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