Mass loss by stars at the stage of the asymptotic giant branch
For a given initial stellar mass function, star formation function, and initial chemical composition, distributions have been constructed for stars of the asymptotic giant branch by luminosity, and for white dwarfs by mass, by calculating the approximate evolution of a large number of stars. Variants are calculated with different assumptions about the mass loss in the asymptotic branch. Theory can be reconciled with observation only if it is assumed that at this stage there is also a still large mass loss in addition to the stellar wind and the ejection of a planetary nebula shell. This provides the explanation for the absence in the Magellanic clouds of carbon stars with M /sub bol/ < -6 /sup m/, the narrow mass distribution of white dwarfs, and the small number of white dwarfs with M > 1.0M /sub ./. The degenerate carbon-oxygen nuclei of stars evolving along the asymptotic giant branch cannot attain the Chandrasekhar limit on account of the great mass loss by the stars. The luminosity of stars of the asymptotic giant branch in the globular clusters of the Magellanic Clouds is a good indicator of the age of the clusters.
- Research Organization:
- Radioastrophysical Observ., Latvian SSR Acad. of Sci.
- OSTI ID:
- 6932948
- Journal Information:
- Astrophysics (Engl. Transl.); (United States), Journal Name: Astrophysics (Engl. Transl.); (United States) Vol. 24:1; ISSN ATPYA
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BOUNDARY CONDITIONS
DWARF STARS
GALAXIES
GIANT STARS
LOSSES
LUMINOSITY
MAGELLANIC CLOUDS
MASS
NEBULAE
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
PLANETARY NEBULAE
STAR CLUSTERS
STAR EVOLUTION
STARS
STELLAR ACTIVITY
STELLAR WINDS
WHITE DWARF STARS