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On the Spectral Classification of Cool White Dwarfs

Published online by Cambridge University Press:  14 August 2015

I. Bues
I. Bues*
Affiliation:
I. Mathematisches Institut der Freien Universität Berlin

Abstract

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The Eggen-Greenstein (1965) classification of cool white dwarfs (DC, DF, DG, λ 4670, λ 4135) was based on the features visible in the spectra of low dispersion. Detailed model atmosphere computations (11000 ≥ Teff ≥ 7000 K) and comparison with spectra observed by Wegner (1974, 1975) show that the variety of the spectra is due to changes in the abundance ratios of C/O, C/H and H/He only. Thus the relative strengths of the C2 and CH-bands can be used for classification and guess of Teff in the range of Teff ≥ 6000 K.

Type
Part I/Influence of Abundances Upon Stellar Atmosphere Calculations
Information
Symposium - International Astronomical Union , Volume 72: Abundance Effects in Classification , 1976 , pp. 23 - 24
Copyright
Copyright © Reidel 1976 

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