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 conference › Poster › Other

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 2010 → 20 Aug 2010

Conference

ConferenceConference on Why Galaxies Care About AGB Stars II (2010)
CountryAustria
CityVienna
Period16/08/10 → 20/08/10

Cite this

Angelou, G. C., Lattanzio, J. C., Church, R. P., Stancliffe, R. J., Dearborn, D. S., Smith, G. H., ... Smith, V. V. (2011). Thermohaline Mixing and the CN Bimodality in M3. Poster session presented at Conference on Why Galaxies Care About AGB Stars II (2010), Vienna, Austria.
Angelou, G C ; Lattanzio, J C ; Church, R P ; Stancliffe, R J ; Dearborn, D S ; Smith, G H ; Tout, C A ; Smith, V V. / Thermohaline Mixing and the CN Bimodality in M3. Poster session presented at Conference on Why Galaxies Care About AGB Stars II (2010), Vienna, Austria.2 p.
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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 ~ 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",

}

Angelou, GC, Lattanzio, JC, Church, RP, Stancliffe, RJ, Dearborn, DS, Smith, GH, Tout, CA & Smith, VV 2011, 'Thermohaline Mixing and the CN Bimodality in M3' Conference on Why Galaxies Care About AGB Stars II (2010), Vienna, Austria, 16/08/10 - 20/08/10, .

Thermohaline Mixing and the CN Bimodality in M3. / Angelou, G C; Lattanzio, J C; Church, R P; Stancliffe, R J; Dearborn, D S; Smith, G H; Tout, C A; Smith, V V.

2011. Poster session presented at Conference on Why Galaxies Care About AGB Stars II (2010), Vienna, Austria.

Research output: Contribution to conference › Poster › Other

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

ER -

Angelou GC, Lattanzio JC, Church RP, Stancliffe RJ, Dearborn DS, Smith GH et al. Thermohaline Mixing and the CN Bimodality in M3. 2011. Poster session presented at Conference on Why Galaxies Care About AGB Stars II (2010), Vienna, Austria.

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