Mass Loss In M67 Giants: Evidence From Isochrone Fitting

We present a study of the stellar content of the open cluster M67. We have computed new evolutionary sequences of stellar models with solar abundance that cover all phases of evolution from the Zero-Age Main Sequence to the bright end of the Asymptotic Giant Branch (AGB). We examine the fit between the calculated and the observed red giant branch (RGB) in particular, and discuss factors that most influence its quality. The distinct color gap between the RGB and the clump giants is compared with the temperature gap between the He-burning tracks and the computed 5 Gyr isochrone. This purely differential approach strongly indicates that the clump giants have M \lta 0.70\msun\ , implying an amount of mass loss ($\approx 0.6$ \msun) well in excess of that found in globular cluster stars. Observational constraints on mass loss processes favor the interpretation that mass loss in cool low-mass giant stars increases with metallicity.Comment: 21pp., plain TeX astro-ph/yymmnn

Derived Parameters for NGC 6791 from High-Metallicity Isochrones

We have computed 8, 10, and 12 Gyr isochrones and physically consistent models of zero-age red horizontal branch stars for stellar masses between 0.55 and 1.3~\msun, all at [Fe/H] $=+0.15$. Comparison to the NGC 6791 BVI photometry of Ka{\l}u\.zny & Udalski (1992) and Montgomery, Janes & Phelps (1994) yields an age of $10.0\pm0.5$ Gyr at an apparent distance modulus 13.49 < \dmv < 13.70. The color offsets required to fit the isochrones, combined with the spectroscopic results of Friel & Janes, imply that the foreground reddening to NGC 6791 lies in the range 0.24 > \ebv >0.19 with $+0.27 <$ [Fe/H] $<+0.44$. The zero-age horizontal branch models suggest that the red horizontal branch stars of NGC 6791 have masses \lesssim 0.7\msun. The masses are similar to those found for M67 red clump stars by Tripicco, Dorman & Bell (1993) and for globular cluster red horizontal branch stars, despite higher and lower masses (respectively) in those cases. This suggests the presence of a mechanism that tends to reduce stellar envelopes on the zero-age horizontal branch {\it to} a given mass rather than {\it by} a given amount.Comment: 23 pages, postscript fil