A proposed observational test of the temperature structure in hot stellar atmospheres

Details A proposed observational test of the temperature structure in hot stellar atmospheres A proposed observational test of the temperature structure in hot stellar atmospheres

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982pazh....8..485s&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 8, Aug. 1982, p. 485-487) Soviet Astronomy Letters (ISSN 0360-0327), vol. 8, July-Aug.

Astronomy and Astrophysics

Astronomy

Carbon Stars, Hot Stars, Stellar Atmospheres, Stellar Temperature, Atomic Spectra, Radiative Transfer, Resonance Lines, Spectral Energy Distribution, Spectral Line Width, Stellar Spectra, Thermodynamic Equilibrium, Ultraviolet Spectra

Scientific paper

A non-LTE calculation in which the equations of transfer and statistical equilibrium for the C IV ion are solved simultaneously reveals that the profile of the 1550 A resonance doublet could be used as an observational test to detect the temperature rise in the outer layers of a star predicted theoretically by current model atmospheres. The C IV lines of carbon in the ultraviolet and visual spectral regions are investigated using Mihalas' models (1972). The non-LTE approach is employed to calculate theoretical line intensities.

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