Flare heating and ionization of the low solar chromosphere. I - Inversion methods for MG I 4571 and 5173

Details Flare heating and ionization of the low solar chromosphere. I - Inversion methods for MG I 4571 and 5173 Flare heating and ionization of the low solar chromosphere. I - Inversion methods for MG I 4571 and 5173

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...350..463m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 350, Feb. 10, 1990, p. 463-474.

Astronomy and Astrophysics

Astrophysics

26

Chromosphere, Solar Electrons, Solar Flares, Solar Spectra, Atmospheric Heating, Electron Density Profiles, Fredholm Equations, Inversions, Line Spectra

Scientific paper

Various methods of inverting solar Mg I 4571 and 5173 spectral line observations are examined to find the best method of using these lines to calculate the vertical temperature and electron density structure around the temperature minimum region. Following a perturbation analysis by Mein (1971), a Fredholm integral equation of the first kind is obtained which can be inverted to yield these temperature and density structures as a function of time. Several inversion methods are tested and compared. The methods are used to test data as well as to a subset of observations of these absorption lines taken on February 3, 1986 before and during a solar flare. A small but significant increase is found in the temperature and a relatively large increase in the electron density during this flare. The observations are inconsistent with heating and ionization by an intense beam of electrons and with ionization by UV photoionization of Si I.

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