Energy balance in the solar transition region. III - Helium emission in hydrostatic, constant-abundance models with diffusion

Details Energy balance in the solar transition region. III - Helium emission in hydrostatic, constant-abundance models with diffusion Energy balance in the solar transition region. III - Helium emission in hydrostatic, constant-abundance models with diffusion

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...406..319f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 406, no. 1, p. 319-345.

Astronomy and Astrophysics

Astrophysics

316

Chromosphere, Emission Spectra, Helium, Solar Corona, Solar Radiation, Astronomical Models, Hydrostatics, Particle Diffusion, Solar Limb

Scientific paper

In our previous papers we described the mathematical formalism and the computed results for energy-balance hydrostatic models of the solar transition region. In this paper we discuss in some detail the limitations of the hydrostatic and one-dimensional assumptions used. Then we analyze the determination of helium emission when diffusion is included. We use transport coefficients estimated from kinetic theory to determine the helium departures from local ionization balance. We calculate the helium spectra for each of our models and evaluate the role of helium in the energy transport. Also, we investigate the effects of coronal illumination on the structure of the transition region and upper chromosphere, and show how coronal illumination affects various EUV lines and the He I 10830 A line. Comparing with both absolute intensities and detailed line profiles, we show that our models are consistent not only with the observed hydrogen spectra but also with the available helium spectra.

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