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Solar Wind and Interplanetary Medium

  • L. Svalgaard
Part of the Astrophysics and Space Science Library book series (ASSL, volume 69)

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.

Keywords

Solar Wind Coronal Hole Interplanetary Magnetic Field Magnetic Field Line Solar Wind Speed 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© D. Reidel Publishing Company, Dordrecht, Holland 1977

Authors and Affiliations

  • L. Svalgaard

There are no affiliations available

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