High-luminosity single carbon stars in stellar and galactic evolution |
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| Authors: | M Jura |
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| Institution: | (1) Astronomy Department, UCLA, 90024 Los Angeles, CA, USA |
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| Abstract: | Summary In the solar neighborhood, approximately half of all intermediate mass main sequence stars with initially between 1 and about 5 M become carbon stars with luminosities near 104 L for typically less than 106 years. These high luminosity carbon stars lose mass at rates nearly always in excess of 10–7 M yr–1 and sometimes in excess of 10–5 M yr–1. 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 importan t in the outer than in the inner Galaxy. |
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| Keywords: | Stars: carbon stars: circumstellar matter stars: evolution of stars: mass loss |
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