Carbon Abundance among Sub-Dwarf Stars in M92

Details Carbon Abundance among Sub-Dwarf Stars in M92 Carbon Abundance among Sub-Dwarf Stars in M92

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop..383b&link_type=abstract

NOAO Proposal ID #2000A-0383

Physics

Scientific paper

A serious discrepancy exists between theories of deep mixing in globular cluster red giant stars and observational evidence. The observed luminosity function of three co-added clusters (including M92) has a local maximum near M_V=-0.4. However, our recent analysis of KPNO Hydra observations of M92 red giant stars indicates that carbon depletion sets in at absolute magnitudes at least as faint as M_V=+0.5 to +1.0, well below that of the local LF peak (Bellman et al., 1999). According to theories of deep stellar mixing, carbon depletion should not become evident until after the LF peak. In order to further constrain mixing theory development, we propose obtaining moderate resolution spectra of stars with M_V > +1.0 in order to establish a baseline carbon abundance for ''unmixed'' stars in M92 and to pinpoint the magnitude at which carbon depletion commences.

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