Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26arv...2..227j&link_type=abstract
Astronomy and Astrophysics Review (ISSN 0935-4956), vol. 2, April 1991, p. 227-247. NASA-supported research.
Astronomy and Astrophysics
Astrophysics
30
Carbon Stars, Galactic Evolution, Stellar Evolution, Stellar Luminosity, Main Sequence Stars, Spatial Distribution, Stellar Composition, Stellar Mass
Scientific paper
In the solar neighborhood, approximately half of all intermediate mass main sequence stars with initially between 1 solar mass and about 5 solar masses become carbon stars with luminosities near 10,000 lunar luminosities for typically less than 1 million years. These high luminosity carbon stars lose mass at rates nearly always in excess of 10 to the -7th solar mass/yr and sometimes in excess of 0.00001 solar mass/yr. Locally, close to half of the mass returned into the interstellar medium by intermediate mass stars before they become white dwarfs is during the carbon star phase. A much greater fraction of lower metallicity stars become carbon-rich before they evolve into planetary nebulae, than do higher-metallicity stars; therefore, carbon stars are much more important in the outer than in the inner Galaxy.
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