Abstract
The goal in this chapter is to discuss the methods of determining the effective temperature of central stars. This temperature is defined in terms of the total flux, integrated over all wavelengths, per unit area of the stars surface. This is very difficult to determine directly from the available data because for the majority of the stars most of the energy is in the inaccessible ultraviolet. Therefore various kinds of evidence are combined in order to best estimate the temperature. The individual sections describe in turn: (A) the line spectra of the stars, (B) the continuous spectra of the stars, (C) model atmospheres which have been constructed to explain these spectra, (D) the stellar temperature determined from the extent of the ionization of the hydrogen and helium in the nebula (‘Zanstra’ temperatures), (E) the energy balance in the nebula (‘Stoy’ temperature) and (F) the stellar temperature determined from the degree of ionization of the various elements in the nebula.
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© 1984 D. Reidel Publishing Company, Dordrecht, Holland
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Pottasch, S.R. (1984). The Temperature of the Central Stars. In: Planetary Nebulae. Astrophysics and Space Science Library, vol 107. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7233-9_7
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DOI: https://doi.org/10.1007/978-94-009-7233-9_7
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