Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977ap%26ss..51..135y&link_type=abstract
Astrophysics and Space Science, vol. 51, no. 1, Sept. 1977, p. 135-152.
Astronomy and Astrophysics
Astrophysics
1
Galactic Nuclei, Planetary Nebulae, Stellar Evolution, Stellar Mass Ejection, Astronomical Models, Cosmology, Galactic Evolution, White Dwarf Stars
Scientific paper
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
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