Abstract
ABSTRACT Evolutionary calculations are presented for three 29M0 configurations, two having super- helium -rich compositions, (X, Y, Z) = (0.30, 0.69, 0.01) and (0.30, 0.695, 0.005), and one a moderately helium-rich composition (0.60, 0.39, 0.01). The Z = 0.005 configuration is evolved past core helium exhaustion, the others only past core helium ignition. Neither super-helium-rich star passes through a significant convective-envelope (Hayashi) phase, either before or after core helium ignition. Both stars become substantially brighter after shell hydrogen ignition and after core helium ignition. The configuration evolved through core helium exhaustion becomes very blue (up to Te = 56,800 K) and very bright (Mb0l -5). The structural evolution of these models is discussed with regard to general ideas on post-main-sequence evolution. Observable features of a hypothetical super-helium-rich cluster are also indicated. Key words: stellar evolution - helium abundance - super -helium -rich stars
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