Abstract The dissipation of solar wind energy makes an important contribution to the energy budget of the earth's upper atmosphere. Heating and momentum transfer by this energy source generate a permanent disturbance zone in the polar region which is characterized by an increase in the temperature and pressure, strong vertical and horizontal winds, and significant changes in the density structure. Heavier gases like Ar, O2 and N2 are enhanced, He depleted, and O moderately enhanced or depleted depending on the altitude. The extension and latitudinal structure of this disturbance zone sensitively depend on a number of parameters including the level of magnetic activity, the season, local, universal and storm time, and solar activity. The same parameters also determine the magnitude of the perturbation. Changes outside the disturbance zone are relatively small and are characterized by an increase of all gas constituents. Whereas present models do provide a first order description, more sophisticated algorithms are needed for a satisfactory representation of the disturbance effects.
Solar wind energy dissipation in the upper atmosphere
Advances in Space Research ; 3 , 1 ; 55-66
1983-01-01
12 pages
Article (Journal)
Electronic Resource
English
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