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

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.

Lattanzio, John C.Monash University (author)
Church, Ross P.Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science,Monash University(Swepub:lu)astr-rch (author)
Stancliffe, Richard J.Monash University (author)
Dearborn, David S.Lawrence Livermore National Laboratory (author)
Smith, Graeme H.University of California, Santa Cruz (author)
Tout, Christopher A.University of Cambridge (author)
Smith, Verne V.National Optical Astronomy Observatory (author)
Monash UniversityAstronomi - Genomgår omorganisation (creator_code:org_t)

In:11th Symposium on Nuclei in the Cosmos, NIC 2010; Heidelberg; Germany; 19 July 2010 through 23 July 2010

By the author/editor: Angelou, George ...; Lattanzio, John ...; Church, Ross P.; Stancliffe, Rich ...; Dearborn, David ...; Smith, Graeme H.; show more...; Tout, Christophe ...; Smith, Verne V.; show less...

About the subject

NATURAL SCIENCES: NATURAL SCIENCES; and Physical Science ...; and Astronomy Astrop ...

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