The Chemical Inhomogeneity of Faint M13 Stars: C and N Abundances

Abstract

Building upon earlier observations which demonstrate substantial star-to-star differences in the carbon abundances of M13 subgiants, we present new Keck LRIS spectra reaching more that 1.5 mag below the M13 main-sequence turn-off (to V ~ 20). Our analysis reveals a distribution of C abundances similar to that found among the subgiants, implying little change in the compositions of the M13 stars at least through the main-sequence turn-off. We presume these differences to be the result of some process operating early in the cluster history. Additional spectra of previously studied bright M13 giants have been obtained with the Hale 5-m. A comparison of C abundances derived using the present methods and those from the literature yield a mean difference of 0.03+-0.14 dex for four stars in common with Smith et al. (1996) and 0.14+-0.07 dex for stars also observed by Suntzeff (1981) (if one extreme case is removed). We conclude that the lower surface C abundances of these luminous giants as compared to the subgiants and main-sequence stars are likely the result of mixing rather than a difference in our abundance scales. NH band strengths have also been measured for a handful of the most luminous M13 turn-off stars. While molecular band formation in such stars is weak, significant star-to-star NH band strength differences are present. Moreover, for the stars with both C and N measurements, differences between stars in these two elements appear to be anticorrelated. Finally, the most recent C and N abundances for main-sequence, main-sequence turn-off, and subgiant stars in 47 Tuc, M71, M5, and the present M13 data are compared.

To be published in The Astronomical Journal (March 2004)

References in corpus (6)

• CN abundance variations on the main sequence of 47 Tuc
• Abundances in Stars from the Red Giant Branch Tip to Near the Main Sequence Turn Off in M5
• The Abundance Evolution of Oxygen, Sodium and Magnesium in Extremely Metal-Poor Intermediate Mass Stars: Implications for the Self-Polution Scenario in Globular Clusters
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