Theoretical chromospheric flare spectra. I. Hydrogen equilibrium for the kinematic flare-shock model of Nakagawa et al. (1973)

Journal Article · Tue Jan 01 04:00:00 EST 1974 · Solar Phys., v. 34, no. 1, pp. 193-206

OSTI ID:4329233

Canfield, R C; Athay, R G

The equations of radiative transfer and statistical equilibrium are solved simultaneously for a model hydrogen atom including Lyman- alpha , Lyman- BETA , Balmer- alpha . and the Lyman, Balmer, and Paschen continua. The model atmospheres are the results of Nakagawa et al. (1973) for a kinematic model of the chromospheric solar flare. It is found that the models adequately predict the total intensity of B alpha , its wing broadening, the presence of a redshifted wing, the maximum electron density, the total line-ofsight second- level population, and the narrowness in height of the B alpha emitting region. The profile of B alpha is strongly self-reversed, however, and agrees with observations only in the presence of 40 to 70 km s/sup -1/ macroturbulent motion. It is found that Nakagawa et al. (1973) seriously overestimate the radiative loss function, which will have a large effect on their models. Proper radiative loss calculations must be included in any physically realistic model. (auth)

• Research Organization: Sacramento Peak Observatory, Sunspot, NM
• NSA Number: NSA-29-030367
• OSTI ID: 4329233
• Journal Information: Solar Phys., v. 34, no. 1, pp. 193-206, Journal Name: Solar Phys., v. 34, no. 1, pp. 193-206; ISSN SLPHA
• Country of Publication: Country unknown/Code not available
• Language: English

Related Subjects

*SOLAR FLARES-- SPECTRA
BALMER LINES
CHROMOSPHERE
ELECTRON DENSITY
HYDROGEN
LYMAN LINES
N56400* --Physics (Astrophysics & Cosmology)--Solar Phenomena
PASCHEN LINES