Late stages of stellar evolution. III - The observed evolution of central stars of planetary nebulae

Details Late stages of stellar evolution. III - The observed evolution of central stars of planetary nebulae Late stages of stellar evolution. III - The observed evolution of central stars of planetary nebulae

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...169..189s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 169, no. 1-2, Nov. 1986, p. 189-193.

Astronomy and Astrophysics

Astrophysics

22

Late Stars, Planetary Nebulae, Stellar Evolution, Asymptotic Giant Branch Stars, Stellar Composition, Stellar Luminosity, White Dwarf Stars

Scientific paper

The evolution of central stars of planetary nebulae has been studied by means of a new distance-independent method. Using Kaler's (1983) sample of large planetary nebulae, it is shown that the distribution of the nebular excitation, which is distance-independent, is well-correlated with the luminosity function of their central stars in that low-excitation nebulae have intrinsically faint central stars, whereas the bright central stars belong to the highly excited nebulae. These observations indicate a very fast luminosity decrease and can be explained only by post-AGB evolutionary models which burn hydrogen in a shell. Consequently, PN-formation must occur preferentially during the quiescent hydrogen burning phase at the tip of the AGB, thus confirming earlier results of Schoenberner (1981). An estimate of the fraction of those central stars that burn mainly helium is also given. The fraction was found to be smaller than 25 percent.

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