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

Angelou, George C. ; Lattanzio, John C. ; Church, Ross P. LU orcid ; Stancliffe, Richard J. ; Dearborn, David S. ; Smith, Graeme H. ; Tout, Christopher A. and Smith, Verne V. (2010) 11th Symposium on Nuclei in the Cosmos, NIC 2010 In Proceedings of Science
Abstract

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.

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organization
publishing date
type
Chapter in Book/Report/Conference proceeding
publication status
published
subject
host publication
11th Symposium on Nuclei in the Cosmos, NIC 2010; Heidelberg; Germany; 19 July 2010 through 23 July 2010
series title
Proceedings of Science
conference name
11th Symposium on Nuclei in the Cosmos, NIC 2010
conference location
Heidelberg, Germany
conference dates
2010-07-19 - 2010-07-23
external identifiers
  • scopus:84887497325
language
English
LU publication?
yes
id
4e09f8d4-db7c-4843-aab3-6936a436db21
date added to LUP
2019-06-05 14:21:09
date last changed
2025-04-04 15:14:13
@inproceedings{4e09f8d4-db7c-4843-aab3-6936a436db21,
  abstract     = {{<p>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.</p>}},
  author       = {{Angelou, George C. and Lattanzio, John C. and Church, Ross P. and Stancliffe, Richard J. and Dearborn, David S. and Smith, Graeme H. and Tout, Christopher A. and Smith, Verne V.}},
  booktitle    = {{11th Symposium on Nuclei in the Cosmos, NIC 2010; Heidelberg; Germany; 19 July 2010 through 23 July 2010}},
  language     = {{eng}},
  month        = {{12}},
  series       = {{Proceedings of Science}},
  title        = {{Thermohaline mixing and the variation of [C/Fe] with magnitude in M3}},
  year         = {{2010}},
}