Smith (2002) and Smith & Martell (2003) have compiled from various sources carbon and nitrogen observations along the giant branch of M3. This has provided us with a dataset to test our understanding of thermohaline mixing (see Eggleton, Dearborn, & Lattanzio 2006, 2008; Charbonnel & Zahn 2007). We match carbon depletion as a function of (absolute) visual magnitude for M3. We also include nitrogen as an extra tracer. We employ the same thermohaline prescription as Ulrich (1972), Kippenhahn et al. (1980), and Charbonnel & Zahn (2007), and we vary the dimensionless free parameter Ct. Kippenhahn et al. (1980) favour Ct= 12, corresponding to a slow, traditional “bloblike” kind of mixing. Ct= 1000 produces the faster mixing favoured by Charbonnel & Zahn (2007) and corresponds to finger-like structures with α ~ 6.
|Number of pages||2|
|Publication status||Published - 2011|
|Event||Conference on Why Galaxies Care About AGB Stars II (2010): Shining Examples and Common Inhabitants - University Campus, Vienna, Vienna, Austria|
Duration: 16 Aug 2010 → 20 Aug 2010
|Conference||Conference on Why Galaxies Care About AGB Stars II (2010)|
|Period||16/08/10 → 20/08/10|