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

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

School of Mathematics

Research output: Contribution to conference › Poster

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 language	English
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	Conference on Why Galaxies Care About AGB Stars II (2010)
Country/Territory	Austria
City	Vienna
Period	16/08/10 → 20/08/10

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Cite this

@conference{40bd56cbf9304ccca31389b5a69d0e43,

title = "Thermohaline Mixing and the CN Bimodality in M3",

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 \textasciitilde{} 6.",

author = "Angelou, \{G C\} and Lattanzio, \{J C\} and Church, \{R P\} and Stancliffe, \{R J\} and Dearborn, \{D S\} and Smith, \{G H\} and Tout, \{C A\} and Smith, \{V V\}",

year = "2011",

language = "English",

note = "Conference on Why Galaxies Care About AGB Stars II (2010) : Shining Examples and Common Inhabitants ; Conference date: 16-08-2010 Through 20-08-2010",

}

TY - CONF

T1 - Thermohaline Mixing and the CN Bimodality in M3

AU - Angelou, G C

AU - Lattanzio, J C

AU - Church, R P

AU - Stancliffe, R J

AU - Dearborn, D S

AU - Smith, G H

AU - Tout, C A

AU - Smith, V V

PY - 2011

Y1 - 2011

N2 - 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.

AB - 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.

M3 - Poster

T2 - Conference on Why Galaxies Care About AGB Stars II (2010)

Y2 - 16 August 2010 through 20 August 2010

ER -