On the chromosphere of 32 Cygni

Details On the chromosphere of 32 Cygni On the chromosphere of 32 Cygni

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....105.1525e&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 105, no. 4, p. 1525-1536.

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Chromosphere, Stellar Spectra, Stellar Spectrophotometry, Stellar Temperature, Temperature Distribution, Zeta Aurigae Star, Astronomical Models, Atmospheric Turbulence, Density Distribution, Doppler Effect, Electron Density (Concentration), H Alpha Line, Iue, K Lines, Spectrum Analysis, Stellar Winds, Ultraviolet Spectroscopy

Scientific paper

Archival IUE observations and new optical spectra of atmospheric eclipses are analyzed to define the physical properties of the chromosphere of 32 Cyg. Excitation temperatures clearly rise with height in the chromosphere, starting at about 5000 K close to the star. Temperatures in the range 12,000-17,000 K are attained high in the chromosphere, although these high values may represent condensations in the wind. Electron density, derived from ionization of Fe, Mg, C, N, S, and Ca, seems to be 10 exp 8-10 exp 9/cu cm throughout the chromosphere. H-alpha must be formed in an extended shell, as in the other Zeta Aur systems, with the line core formed at a level where the wind is beginning to dominate the static chromosphere. We compare the temperature-mass distributions for Zeta Aur binaries with semiempirical chromospheric models and find they are really very different. Not only are measured temperatures higher than in the models, but the increased electron densities imply a somewhat different distribution of emission and mass density relative to such homogeneous models.

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