Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...138..333c&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 138, no. 2, Sept. 1984, p. 333-336. Sponsorship: Deutsche Forschungsgemeinscha
Astronomy and Astrophysics
Astrophysics
10
K Stars, Plasma Temperature, Stellar Spectra, Stellar Winds, Supergiant Stars, Ultraviolet Spectra, Iron, Line Shape, Radiative Transfer, Stellar Temperature
Scientific paper
This paper is an attempt to determine the wind temperature of cool supergiants empirically, independent of wind models. Fe II P-Cygni lines from the first excitation levels have been detected in the line spectra of Zeta Aurigae and VV Cephei binary systems. These lines are formed in the winds of the cool supergiants. The Zeta Aurigae system 32 Cyg has been chosen for this investigation due to the high quality of spectra at various characteristic phases. Radiative transfer analysis of the lines enables to determine the population densities of the lowest excitation levels, which are then compared with existing model calculations to deduce the excitation temperature. The lower limit of the excitation temperature is found to be 4200K (LTE population) in the Fe II line-formation zone. When less than 1% of the circumstellar matter is ionized Te ≡ O(104K) is to be expected.
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