Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...122..314t&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 122, no. 1-2, June 1983, p. 314-321. Sponsorship: Deutsche Forschungsgemeinsch
Astronomy and Astrophysics
Astrophysics
11
Giant Stars, H Lines, Infrared Spectra, M Stars, Stellar Spectra, Abundance, Molecular Spectra, Quadrupoles, Red Giant Stars, Stellar Atmospheres, Stellar Models
Scientific paper
The H2 quadrupole line in the spectra of cool stars could be a sensitive probe of the atmospheric structure of these stars. This possibility is examined in M-giant stars. The predicted line profiles of H2 quadrupole lines based on the line-blanketed model atmospheres turn out to be too strong as compared with the observed H2 lines. The most likely explanation may be that the outer layers of M-giant stars are hotter by more than 100K as compared with the predictions based on line-blanketed model atmospheres. The results for M-giant stars is compared with the recent results for S- and C-type stars. Predicted line intensities for oxygen-rich giant stars show that H2 lines are much stronger in S-type model atmospheres than in M-type model atmospheres. This result is consistent with recent observations. This means that classical model atmospheres of oxygen-rich giant stars reasonably represent the differential line-blanketing effect between M- and S-type stars.
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