Thermohaline mixing and the variation of [C/Fe] with magnitude in M3

George C. Angelou, John C. Lattanzio, Ross P. Church, Richard J. Stancliffe, David S. Dearborn, Graeme H. Smith, Christopher A. Tout, Verne V. Smith

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We use observations of M3 to constrain thermohaline mixing. This is done by matching [C/Fe] and [N/Fe] along the RGB of M3. We find our models can explain observations if it is assumed there is a spread of ∼ 0.3 - 0.4 dex in [C/Fe] in the stars in M3 from their birth. We reproduce the full spread in [C/Fe] at the tip of the RGB. Thermohaline mixing can produce a significant change in [N/Fe] as a function of absolute magnitude on the RGB for initially CN-weak stars, but not for initially CN-strong stars, which have so much nitrogen to begin with that any deep mixing does not significantly affect the surface nitrogen composition.

Original languageEnglish
JournalProceedings of Science
Publication statusPublished - 1 Dec 2010
Event11th Symposium on Nuclei in the Cosmos, NIC 2010 - Heidelberg, Germany
Duration: 19 Jul 201023 Jul 2010

Cite this

Angelou, G. C., Lattanzio, J. C., Church, R. P., Stancliffe, R. J., Dearborn, D. S., Smith, G. H., Tout, C. A., & Smith, V. V. (2010). Thermohaline mixing and the variation of [C/Fe] with magnitude in M3. Proceedings of Science.