Late stages of stellar evolution. II. Mass loss and the transition of asymptotic giant branch stars into hot remnants

Journal Article · Thu Sep 15 04:00:00 EDT 1983 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/161333· OSTI ID:5474977

Schoenberner, D

We have computed the transition of asymptotic branch giants of 0.8 and 1.0 M/sub sun/ into remnants of 0.565, 0.553, and 0.546 M/sub sun/ by means of mass loss which removed the stellar envelopes in about 10/sup 3/ yr. The remnants were then evolved across the H-R diagram to the white dwarf configuration and their relevance for central stars of planetary nebulae studied. From the temporal evolution of these models we determined lower limits for mass and luminosity of central stars of approx.0.55 M/sub sun/ and approx.2500 L/sub sun/.

• Research Organization: Louisiana State University Observatory
• OSTI ID: 5474977
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 272:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
DIAGRAMS
DWARF STARS
GIANT STARS
HERTZSPRUNG-RUSSELL DIAGRAM
NEBULAE
PLANETARY NEBULAE
PULSATIONS
STAR BURNING
STAR EVOLUTION
STARS
STELLAR WINDS
WHITE DWARF STARS