Post-asymptotic giant branch nonradial instability strips

Journal Article · Sun Dec 01 04:00:00 EST 1991 · Astrophysical Journal; (United States)

DOI:https://doi.org/10.1086/170835· OSTI ID:5813242

Stanghellini, L; Cox, A N; Starrfield, S ^[1]

---

1. Osservatorio Astronomico, Bologna (Italy) Los Alamos National Laboratory, NM (United States) Arizona State University, Tempe (United States)

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. 51 refs.

• OSTI ID: 5813242
• Journal Information: Astrophysical Journal; (United States), Journal Name: Astrophysical Journal; (United States) Vol. 383; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

661300* -- Other Aspects of Physical Science-- (1992-)
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COMPARATIVE EVALUATIONS
DIAGRAMS
DWARF STARS
EVALUATION
HERTZSPRUNG-RUSSELL DIAGRAM
MASS
MASS TRANSFER
MATHEMATICAL MODELS
NEBULAE
OSCILLATIONS
PLANETARY NEBULAE
STABILITY
STAR CLUSTERS
STAR EVOLUTION
STAR MODELS
STARS
VARIABLE STARS
WHITE DWARF STARS