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Theory of Evolution of Central Stars of Planetary Nebulae

Published online by Cambridge University Press:  22 September 2016

B. Paczyński
B. Paczyński*
Affiliation:
Princeton University Observatory and N. Copernicus Astronomical Center, Polish Academy of Sciences

Abstract

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Young central stars of planetary nebulae burn hydrogen and helium in the shell sources. Within less than 104 years nuclear fuel is exhausted and old central stars cool off at almost constant radius to the white dwarf stage.

Young, i.e., luminous central stars should follow complicated loops on the H-R diagram as a result of helium shell flashes. FG Sagittae is the example. This should be a typical behaviour and a systematic search for light variations on a time scale of years or decades among other luminous entral stars should be undertaken. Because of rapid evolution of their nuclei many planetary nebulae may be far from the ionization equilibrium. This should be taken into account when the effective temperature and bolometric luminosity of the central stars are estimated.

Type
Session IV: The Central Stars of Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 76: Planetary Nebulae , 1978 , pp. 201 - 205
Copyright
Copyright © Reidel 1978 

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