Initial-final mass relation for low and intermediate mass stars

Journal Article · Fri May 01 04:00:00 EDT 1987 · Astrophysics (Engl. Transl.); (United States)

DOI:https://doi.org/10.1007/BF01011229· OSTI ID:5619028

Frantsman, Yu L

An approximate calculation of the evolution of stars of different masses to the white dwarf stage leads to a relation between the initial, M/sub i/, and final, M/sub f/, masses of stars for M/sub i/ in the range 1-8 M/sub circle/ corresponding to different assumptions about the mass loss in the stage of the asymptotic giant branch. It is shown that the M/sub i/-M/sub f/ relation obtained on the basis of mass estimates for the white dwarfs in clusters in our Galaxy (10) is apparently incorrect. Estimates of M/sub i/ and J/sub f/ for the stars for the clusters in the Magellanic Clouds and comparison of these values with the theoretically obtained values show that the rate of mass loss by stars in the Large Magellanic Cloud exceeds the loss rate in the Small Magellanic Cloud. The mass distribution of white dwarfs in galaxies must depend on the initial chemical composition of the stars.

• OSTI ID: 5619028
• Journal Information: Astrophysics (Engl. Transl.); (United States), Journal Name: Astrophysics (Engl. Transl.); (United States) Vol. 25:3; ISSN ATPYA
• 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
CHEMICAL COMPOSITION
DIAGRAMS
DISTRIBUTION
DWARF STARS
ERUPTIVE VARIABLE STARS
GALAXIES
GIANT STARS
HERTZSPRUNG-RUSSELL DIAGRAM
LOSSES
MASS
MASS DISTRIBUTION
MATHEMATICAL MODELS
SPATIAL DISTRIBUTION
STAR CLUSTERS
STAR EVOLUTION
STAR MODELS
STARS
SUPERNOVAE
VARIABLE STARS
WHITE DWARF STARS