A burst model for line emission in the solar atmosphere. II - Coronal extreme ultraviolet lines

Details A burst model for line emission in the solar atmosphere. II - Coronal extreme ultraviolet lines A burst model for line emission in the solar atmosphere. II - Coronal extreme ultraviolet lines

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...398..692f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 398, no. 2, p. 692-697.

Astronomy and Astrophysics

Astrophysics

29

Emission Spectra, Solar Atmosphere, Solar Corona, Solar Radio Bursts, Ultraviolet Spectra, Line Spectra, Plasma Heating, Solar Flares

Scientific paper

We review the spectroscopic evidence for explosive events - bursts - occurring in solar coronal plasmas. Problems in the interpretation of extreme ultraviolet spectra from Mg-like ions, particularly Fe XV in solar flares can be obviated to certain extent if these ions are produced in an ionizing plasma, with the 3s3p 3P levels being excited directly by inner shell ionization of the Al-like ion. We believe that a similar mechanism should apply to Be-like ions. The excitation following inner shell ionization can become important compared to electron impact excitation at a temperature corresponding to approximately twice the ionization potential of the ion concerned, but to be properly effective, it requires some deviation of the electron distribution function from a Maxwellian. The model we present produces a coronal heating rate from these bursts that is somewhat larger than current estimates.

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