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Quantitative spectral analyses of CSPNs of early [WC]-type

Published online by Cambridge University Press:  25 May 2016

L. Koesterke  and
W.-R Hamann
L. Koesterke
Affiliation:
Institut für Theoretische Physik und Astrophysik der Universität Potsdam
W.-R Hamann
Affiliation:
Institut für Theoretische Physik und Astrophysik der Universität Potsdam

Extract

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Among the Central Stars of Planetary Nebulae (CSPN) there are several stars which show Wolf-Rayet-type spectra resembling those of Pop. I Wolf-Rayet (WR) stars of the carbon sequence (WC). Due to progress in computer technology and new solution techniques it became possible ten years ago to calculate models which account for the very complex physical conditions in Wolf-Rayet atmospheres (Hillier 1989, Hamann et al. 1992). These models have been successfully applied to the vast majority of Pop. IWR stars in the Galaxy and the Magellanic Clouds (Hamann et al. 1995) and, in the last three years, to an increasing sample of CSPNs of [WC] type (Koesterke & Hamann 1996, Leuenhagen & Hamann 1996, Leuenhagen this meeting). Here we present the analyses of ten CSPNs of early [WC] type, i.e. from [WC 2] to [WC 4].

Type
III. Central Stars
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 114 - 115
Copyright
Copyright © Kluwer 1997 

References

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