Flare heating and ionization of the low solar chromosphere. II - Observations of five solar flares

Details Flare heating and ionization of the low solar chromosphere. II - Observations of five solar flares Flare heating and ionization of the low solar chromosphere. II - Observations of five solar flares

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...365..391m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 365, Dec. 10, 1990, p. 391-406. Research supported by the Lockheed Independ

Astronomy and Astrophysics

Astrophysics

34

Chromosphere, Line Spectra, Magnesium, Solar Flares, Electric Current, Electron Beams, Goes Satellites, Magnetohydrodynamic Waves, Photosphere, Proton Beams, Solar Maximum Mission, Temperature Distribution, Ultraviolet Radiation

Scientific paper

Two neutral Mg spectral lines formed in the temperature-minimum region and the low chromosphere, at 4571 and 5173 A, are used to quantify the changes in the atmospheric structure as a function of time during five solar flares. Eight proposed flare heating and ionization mechanisms and predictions of the effects of each on the temperature minimum region are discussed. Two Mg spectral observations made at the National Solar Observatory (Sacramento Peak), along with observations of hard and soft X-rays from the SMM and GOES satellites, are compared to the predictions of the eight proposed mechanisms. The initial effects in all five flares are consistent with backwarming by enhanced Balmer- and Paschen-continuum radiation originating in the upper chromosphere. Extended heating observed in two of the flares is most likely due to UV irradiation. In all cases heating by the dissipation of nonreversed electric currents, collisions with an electron or proton beam, irradiation by soft X-rays, and dissipation of Alfven waves are eliminated.

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