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Are Zanstra Temperatures Always Real?

Published online by Cambridge University Press:  19 July 2016

L. H. Aller
L. H. Aller*
Affiliation:
Astronomy Department, University of California, Los Angeles

Abstract

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The classical Zanstra method compares a H Balmer line or He II λ4686 with flux from a limited region of the planetary nuclear (PNN) spectrum to obtain the central star temperature T(PNN). Long ago it was found that generally T(He II) > T(H I), a result attributed to differing optical depths at the Lyman limits of He II and H I; T(He II) often was regarded as the “real” temperature. Much attention has been paid to discordances between Zanstra temperatures and those found by other means, such as the energy-balance (EB) method. (see e.g., Preite-Martinez and Pottasch 1984).

Type
III. Central Stars
Information
Symposium - International Astronomical Union , Volume 131: Planetary Nebulae , 1989 , pp. 306
Copyright
Copyright © Kluwer 1989 

References

Preite-Martinez, A. and Pottasch, S.R. 1983, Astron Astrophys., 126, 31.Google Scholar
Shields, G.A. et al. 1981, Ap. J., 248, 569. [The 1987 references are to papers in this conference].CrossRefGoogle Scholar