Evolutionary versus dynamical time scales for the evolution of the central stars of planetary nebulae

Details Evolutionary versus dynamical time scales for the evolution of the central stars of planetary nebulae Evolutionary versus dynamical time scales for the evolution of the central stars of planetary nebulae

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...351..230m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 351, March 1, 1990, p. 230-244. Research supported by the Max-Planck-Instit

Astronomy and Astrophysics

Astrophysics

48

Asymptotic Giant Branch Stars, Planetary Nebulae, Stellar Evolution, Absorption Spectra, Hertzsprung-Russell Diagram, Photoionization, Stellar Envelopes, Stellar Mass, Stellar Winds

Scientific paper

The disagreement between evolutionary and dynamical time scales for the evolution of the central stars of planetary nebulae (CSPN) through the H-R diagram is investigated. Three possible reasons for the disagreement are examined: (1) the nebulae could have experienced a phase of rapid photoionization of material ejected previously while the stars were still on the AGB; (2) the central stars could have undergone a late helium shell flash and returned to the AGB; and (3) the AGB-CSPN evolutionary transition times could have been increased by small additional amounts of residual envelope material remaining after the superwind mass-loss phase. Mechanism (3) is favored here because it can account for evolutionary ages both less than and greater than the corresponding dynamical ages.

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