Thermohaline Mixing and the CN Bimodality in M3

G C Angelou, J C Lattanzio, R P Church, R J Stancliffe, D S Dearborn, G H Smith, C A Tout, V V Smith

Research output: Contribution to conferencePoster

Abstract

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.
Original languageEnglish
Number of pages2
Publication statusPublished - 2011
EventConference on Why Galaxies Care About AGB Stars II (2010): Shining Examples and Common Inhabitants - University Campus, Vienna, Vienna, Austria
Duration: 16 Aug 201020 Aug 2010

Conference

ConferenceConference on Why Galaxies Care About AGB Stars II (2010)
CountryAustria
CityVienna
Period16/08/1020/08/10

Cite this