Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....79..108s&link_type=abstract
Astronomy and Astrophysics, vol. 79, no. 1-2, Oct. 1979, p. 108-114. Research supported by the Deutsche Forschungsgemeinschaft.
Astronomy and Astrophysics
Astrophysics
304
Asymptotic Giant Branch Stars, Helium, Red Giant Stars, Stellar Evolution, Stellar Mass Ejection, Stellar Envelopes, Stellar Mass, Stellar Models, White Dwarf Stars
Scientific paper
Evolutionary calculations of low mass stars from the beginning of core helium burning to the white-dwarf configuration are presented. During the giant stage, steady mass loss by a stellar wind has been included according to Reimers's (1975) empirical law. While the evolution follows the Hayashi track up to 34 helium shell flashes are encountered. However, the flash-driven convective helium shells do not reach the overlying hydrogen-rich layers because of the high entropy content of the latter. At the tip of the (asymptotic) giant branch mass loss competes with hydrogen burning, which accelerates the blueward evolution and reduces the time for crossing the H-R diagram toward the white-dwarf region to intervals equal to the interflash periods. Therefore fully developed helium shell flashes can occur at effective temperatures higher than 100,000 K.
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