On the evolution of central stars of planetary nebulae

The evolution of nuclei of planetary nebulae has been calculated from the end of the ejection stage that produces the nebulae to the white-dwarf stage. The structure of the central star is in agreement with the general picture of Finzi (1973) about mass ejection from the progenitors of planetary neb...

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Bibliographic Details
Published in:Astrophysics and space science 1977-09, Vol.51 (1), p.135-152
Main Author: Yahel, Raphael Z.
Format: Article
Language:English
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Summary:The evolution of nuclei of planetary nebulae has been calculated from the end of the ejection stage that produces the nebulae to the white-dwarf stage. The structure of the central star is in agreement with the general picture of Finzi (1973) about mass ejection from the progenitors of planetary nebulae. It has been found that in order to obtain an evolutionary track consistent with the Harman-Seaton (1966) track, one has to assume that the masses of the central stars are less than about 0.7 solar mass. The calculated evolutionary time scale of the central stars of planetary nebulae is of the order of 20,000 yr. This time scale is negatively correlated with the stellar mass; the heavier the stellar mass, the shorter the evolutionary time scale
ISSN:0004-640X
1572-946X
DOI:10.1007/BF00642463