The evaluation of the Balmer merging effects in different chromospheric solar flare models.
Abstract
Synthetic spectra computed with semiempirical and theoretical models of the flare atmosphere are discussed. Stark profile of the Balmer lines (n ≥ 6) and the Balmer continuum have been computed according to Donati-Falchi et al., (1985). A semiempirical model in between the F2 and F3 models proposed by Avrett et al., (1986) might represent a good approximation of the atmosphere of a flare during the impulsive phase. Among the theoretical models proposed by Ricchiazzi (1982), the model, indicated as 1073, with very high coronal pressure (Pυ = 1000 dyne cm-2) probably represents the best approximation of the emission observed during the impulsive phase of a chromospheric flare.
- Publication:
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Solar and Stellar Flares. Poster Papers
- Pub Date:
- 1989
- Bibcode:
- 1989sasf.confP.345F
- Keywords:
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- Solar Flares: Synthetic Spectra;
- Solar Flares: Stark Effect