Initial-final mass relation for low and intermediate mass stars

Details Initial-final mass relation for low and intermediate mass stars Initial-final mass relation for low and intermediate mass stars

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986afz....25..517f&link_type=abstract

(Astrofizika, vol. 25, Nov.-Dec. 1986, p. 517-524) Astrophysics (ISSN 0571-7132), vol. 25, no. 3, May 1987, p. 655-660. Translat

Astronomy and Astrophysics

Astrophysics

2

Stellar Evolution, Stellar Mass, Asymptotic Giant Branch Stars, Chemical Composition, Giant Stars, Magellanic Clouds, Mass Distribution, Milky Way Galaxy, Star Clusters, White Dwarf Stars

Scientific paper

The initial-final theoretical mass relations Mi-Mf for low- and intermediate-mass stars are presented and the effect of different assumptions on mass loss is discussed. It appears that Weidemann and Koester (1983) Mi-Mf relations are erroneous. The data on AGB stars in the Magellanic Cloud clusters indicate that the mass loss process is very sensitive to the metal abundance. Mass distributions of white dwarfs must be different in galaxies with different chemical compositions.

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