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The Evaluation of the Balmer Merging Effects in Different Chromospheric Solar Flare Models

Published online by Cambridge University Press:  27 September 2017

A. Falchi ,
R. Falciani ,
L.A. Smaldone  and
G.P. Tozzi
A. Falchi
Affiliation:
Osservatorio Astrofisico di Arcetri, Firenze, Italy
R. Falciani
Affiliation:
Istituto di Astronomia, Universita' di Firenze, Firenze, Italy
L.A. Smaldone
Affiliation:
Dipartim. Sc. Fisiche, Universita' di Napoli, Napoli, Italy
G.P. Tozzi
Affiliation:
Osservatorio Astrofisico di Arcetri, Firenze, Italy

Abstract

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Synthetic spectra computed svith semiempirical and theoretical models of the flare atmosphere are discussed. Stark profile of the Dahner 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 impusive phase. Among the theoretical models proposed by Ricchiazzi (1982), the model, indicated as 1073, with very high coronal pressure (Po = 1000 dyne cm–2) probably represents the best approximation of the emission observed during the impulsive phase of a chromospheric flare. Continuum and Balmer lines ought to be measured and interpreted on the same time for a self-consistent diagnostic of the chromospheric modification.

Type
Session III: Theory
Information
International Astronomical Union Colloquium , Volume 104 , Issue 2: Solar and Stellar Flares , 1989 , pp. 345 - 348
Copyright
Copyright © Kluwer 1989

References

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