Non-Maxwellian electron distributions in models of the solar atmosphere

Details Non-Maxwellian electron distributions in models of the solar atmosphere Non-Maxwellian electron distributions in models of the solar atmosphere

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...369..544m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 369, March 10, 1991, p. 544-548.

Astronomy and Astrophysics

Astrophysics

12

Electron Distribution, Photosphere, Solar Atmosphere, Solar Corona, Solar Electrons, Chromosphere, Hydrogen, Maxwell-Boltzmann Density Function, Stellar Models

Scientific paper

In this paper, the solar models of Fontenla et al. (1990) are extended to coronal temperatures using optically thin radiative losses and a semicircular loop geometry. The effects of a non-Maxwellian high-energy tail of the electron distribution function is tested by performing a Fokker-Planck calculation of the tail. The results show that the downward conductive heat flux is very clsoe to that given by Braginskii (1965) for small departures from a Maxwellian distribution. The effects of the high-energy tail of the electron distribution on element ionization are computed and found to be negligible for all ionization states of O, Ne, and Si. It is concluded that, for quiet sun loop models in stationary energy balance, the ionization state of all elements is not significantly affected by the non-Maxwellian tail of the electron velocity distribution, and that the heat flux can be computed by considering only small first-order departures from the Maxwellian distribution.

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