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Non-LTE analysis of central stars∗

Published online by Cambridge University Press:  04 August 2017

R.P. Kudritzki ,
R.H. Méndez  and
K.P. Simon
R.P. Kudritzki
Affiliation:
Institut für Astronomie und Astrophysik der Universität München, Scheinerstr. 1, D-8000 München 80, Federal Republic of Germany
R.H. Méndez
Affiliation:
Instituto de Astronomia Y Fisica del Espacio, C.C. 67, Suc 28, 1428 Buenos Aires, Argentina Cerro Tololo Inter-American Observatory, operated by the Association of Universities for Research in Astronomy, Inc., under contract with the U.S. National Science Foundation “Carrera del Investigador Cientifico”, Conicet, Argentina
K.P. Simon
Affiliation:
Institut für Astronomie und Astrophysik der Universität München, Scheinerstr. 1, D-8000 München 80, Federal Republic of Germany

Extract

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Most of our present knowledge about central stars of planetary nebulae (CPN) is obtained by indirect methods using the emission line spectra of the surrounding nebula. These methods, which apply the beautiful recombination theory, can provide us with information about temperature, distance and radius of the CPN. However, we know that these methods are subject to severe problems, which then lead to strong discrepancies in the parameters of the CPN.

Type
I. EVOLUTION OF LOW AND INTERMEDIATE MASS STARS OBSERVATIONS AND MODELS
Information
Symposium - International Astronomical Union , Volume 105: Observational Tests of the Stellar Evolution Theory , 1984 , pp. 205 - 208
Copyright
Copyright © Reidel 1984 

References

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