Post-asymptotic giant branch nonradial instability strips

Details Post-asymptotic giant branch nonradial instability strips Post-asymptotic giant branch nonradial instability strips

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...383..766s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 383, Dec. 20, 1991, p. 766-778. Research supported by Los Alamos National L

Astronomy and Astrophysics

Astrophysics

45

Asymptotic Giant Branch Stars, Stellar Evolution, Stellar Models, Stellar Oscillations, White Dwarf Stars, Hertzsprung-Russell Diagram, Planetary Nebulae, Stellar Mass, Stellar Mass Ejection, Stellar Temperature, Variable Stars

Scientific paper

Stability analyses are performed for nonradial g(+)-mode pulsations of postasymptotic AGB stellar models to determine the location of their pulsational instability strips in the Hertzsprung-Russell diagram. Stellar models are analyzed that are assumed to have undergone a major mass loss event either near the tip of the AGB or shortly thereafter and, therefore, consist of a 50-percent carbon 50-percent oxygen core. Their mass is 0.6 solar mass, which is in good agreement with the peak of the observed distribution of white dwarf masses. The results are compared both to the observed planetary nebula nuclei variables and the hot pulsating DO variables. An analysis is also presented of the stability of DB white dwarfs, which have much deeper and stronger convection zones, and an instability strip is found between about 18,000 and 26,000 K approximately as observed for the known variable stars.

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