Non-Maxwellian Velocity Distribution Functions Associated with Steep Temperature Gradients in the Solar Transition Region - Part Two - the Effect of Non-Maxwellian Electron Distribution Functions on Ionization Equilibrium Calculations for Carbon Nitrogen a

Details Non-Maxwellian Velocity Distribution Functions Associated with Steep Temperature Gradients in the Solar Transition Region - Part Two - the Effect of Non-Maxwellian Electron Distribution Functions on Ionization Equilibrium Calculations for Carbon Nitrogen a Non-Maxwellian Velocity Distribution Functions Associated with Steep Temperature Gradients in the Solar Transition Region - Part Two - the Effect of Non-Maxwellian Electron Distribution Functions on Ionization Equilibrium Calculations for Carbon Nitrogen a

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980soph...68..265d&link_type=abstract

Solar Physics, Vol. 68, P. 265, 1980

Physics

17

Scientific paper

Non-Maxwellian electron velocity distribution functions, computed for Dupree's (1972) model of the solar transition region in a previous paper, are used to calculate ionization rates for ions of carbon, nitrogen, and oxygen. Ionization equilibrium populations for these ions are then computed and compared with similar calculations assuming Maxwellian distribution functions for the electrons. The results show that the ion populations change (compared to the values computed with a Maxwellian) in some cases by several orders of magnitude depending on the ion and its temperature of formation.

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