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Spectral Analyses of WC-Type Central Stars

Published online by Cambridge University Press:  07 August 2017


W.-R. Hamann
Affiliation:
Institut für Theoretische Physik und Sternwarte der Universität, Kiel, FRG
L. Koesterke
Affiliation:
Institut für Theoretische Physik und Sternwarte der Universität, Kiel, FRG


Extract

Models have been developed in Kiel for massive (Pop. I) WR stars which account for multi-level non-LTE radiation transfer in spherically expanding atmospheres. The published (Koesterke et al. 1992) grid of models for WC composition (40% helium, 60% carbon by mass) can be applied to low-mass stars as well by means of the scaling properties of WR spectra (Hamann et al. 1992) and allow a rough guess of the parameters, while individual calculations are necessary for a detailed analysis and the determination of the chemical composition.


Type
II. Highlights on the Nuclei
Copyright
Copyright © Kluwer 1993 

References

Hamann, W.-R., Leuenhagen, U., Koesterke, L., Wessolowski, U.: 1992, A&A 255, 200 Google Scholar
Koesterke, L., Hamann, W.-R., Wessolowski, U.: 1992, A&A (in press) Google Scholar
Schönberner, D., Blöcker, T.: 1992, in Atmospheres of Early-type stars , Heber, U. and Jeffery, C.S. (eds.), Lecture Notes in Physics 401, Springer, p. 305 CrossRefGoogle Scholar
Werner, K., Heber, U.:1991, A&A 247, 476 Google ScholarPubMed
Werner, K., Koesterke, L.: 1992, in Atmospheres of Early-type stars , Heber, U. and Jeffery, C.S. (eds.), Lecture Notes in Physics 401, Springer, p. 288 CrossRefGoogle Scholar

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