Abstract
Photoelectron fluxes escaping from the ionosphere into the magnetosphere are calculated including the effect of photoelectron diffusion for a range of solar activity. The method employs a two dimensional matrix of continuity equations. In the region where the mean free path of the photoelectrons is small compared with the scale height the predominant term in the transport equation is the upward diffusion flux. As the altitude increases three components of the flux can be considered, an upward escaping component, an upward non-escaping component and a downward component. The relation between these fluxes, the heating of the protonosphere, and the photoelectron fluxes at the far end of the field line are examined.
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