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Masses of the central stars of Planetary Nebulae

Published online by Cambridge University Press:  25 May 2016

S.K. Górny ,
G. Stasińska  and
R. Tylenda
S.K. Górny
Affiliation:
1Copernicus Astronomical Center, Toruń, Poland
G. Stasińska
Affiliation:
2Observatoire de Meudon, France
R. Tylenda
Affiliation:
1Copernicus Astronomical Center, Toruń, Poland

Extract

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The aim of this study is to derive the masses of the central stars (CSPN) for a large sample of the planetary nebulae (PN). These masses, M ∗, are derived from the observed PN positions in three diagnostic diagrams and their comparison with evolutionary tracks of model PN. Two of the diagrams, namely L Zan(H) versus T Zan(H) and M v versus R neb, have already been used in numerous studies. The third one, S Hβ versus S V, has recently been introduced by Górny, Stasińska & Tylenda (1996, hereinafter GST96). Here S Hβ is the nebular surface brightness in Hβ and S v is defined as F v/(πθ2), where F v is the stellar flux in the V band and θ is the observed nebular angular radius.

Type
III. Central Stars
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 107
Copyright
Copyright © Kluwer 1997 

References

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Górny, S.K., Stasińska, G., Tylenda, R., 1996, A&A in press (GST96).Google Scholar
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