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The Chromospheres of Carbon Stars

Published online by Cambridge University Press:  25 May 2016

Donald G. Luttermoser
Donald G. Luttermoser*
Affiliation:
Department of Physics, East Tennessee State University, Johnson City, TN 37614, U.S.A.

Abstract

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Most oxygen-rich late-type giant stars show evidence for chromospheres in their visual spectra (e.g. Ca ii H & K emission features). Cool (i.e. N-type) non-Mira carbon stars, however, have never been observed to have chromospheric emission in their Ca ii H & K lines. However, faint Mg ii h & k lines were detected in emission in low-dispersion IUE spectra of the brightest cool carbon stars in the early 1980s. May 1984 saw the first (and only) successful high-dispersion IUE spectrum taken of a cool carbon star, TX Psc (N0; C6,2). Armed with this high-dispersion spectrum, as well as low-dispersion IUE and ground-based spectra, Luttermoser et al. (1989) made the first detailed attempt to semiempirically model the chromosphere of a cool carbon star. This model was successful in reproducing the Mg ii lines, but it was not well constrained due to the lack of other observed high-resolution chromospheric profiles for comparison. Modeling carbon star chromospheres can now be addressed more accurately with HST/GHRS high-resolution spectra. New fluoresced emission features have been discovered in the GHRS spectra of carbon stars that are not present in their oxygen-rich counterparts.

Type
Session II — Models and Abundance Determinations
Information
Symposium - International Astronomical Union , Volume 177: The Carbon Star Phenomenon , 2000 , pp. 105 - 114
Copyright
Copyright © Kluwer 2000 

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