Numerical solution of the time-dependent heat energy equations for the magnetosphere

Details Numerical solution of the time-dependent heat energy equations for the magnetosphere Numerical solution of the time-dependent heat energy equations for the magnetosphere

Nov 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979p%26ss...27.1343r&link_type=abstract

Planetary and Space Science, vol. 27, Nov. 1979, p. 1343-1350.

Physics

Atmospheric Heat Budget, Earth Magnetosphere, Electron Energy, Ion Temperature, Numerical Integration, Thermodynamics, Time Dependence, F Region, Hydrogen Ions, Ionospheric Temperature, Positive Ions

Scientific paper

A solution of the magnetospheric heat equations capable of covering the whole region from 300 km along a field line to the equatorial plane has been achieved by adapting the searching procedure of Murphy (1974). It has been found that the protonospheric heat reservoir is sufficient to maintain an electron temperature higher than the neutral temperature down to the height of the F2-peak electron density all through the night at midlatitudes. Full solution of the equations has also shown that the ion temperature is higher than the electron temperature in the protonosphere at night and the ions constitute a significant source of heat for the electrons.

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