Advanced evolutionary phases of low-mass stars: The role of the original helium

Details Advanced evolutionary phases of low-mass stars: The role of the original helium Advanced evolutionary phases of low-mass stars: The role of the original helium

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...297..115b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 297, no. 1, p. 115-126

Astronomy and Astrophysics

Astrophysics

23

Globular Clusters, Helium, Star Formation, Stellar Evolution, Asymptotic Giant Branch Stars, Metallicity, Stellar Luminosity, Stellar Models

Scientific paper

We present evolutionary He burning models which cover both the HB and AGB evolutionary phases, as computed for the metallicities Z = 10-4, 10-3 and for two assumptions on the value of the original He content Y = 0.20, 0.27. We found that both the difference in luminosity between the AGB and the HB, and the number ratio of AGB to HB stars appear quite unaffected by the amount of original He, allowing a relevant test for the efficiency of interal mixing during the central He buring phase. Data concerning HB evolution have been connected with the evolutinary times of the corresponding RGB stars to recalibrate the parameters R as a function of Y for the two investigated metallicities. Comparisons with previous calibrations disclose variations which are not negilbible, and which should be taken into account when R is used to derive constraints on the amount of cosmological helium. The critical role of the HB luminosity on the evaluation of R is briefly discussed.

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