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Cited by 55Stellar, planetary, and galactic studiesGamma-ray bursts and supernovaeGalaxies: Formation, Evolution, Phenomena

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EVOLUTION AND NUCLEOSYNTHESIS OF ASYMPTOTIC GIANT BRANCH STARS IN THREE MAGELLANIC CLOUD CLUSTERS

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Kamath, D., Karakas, A. I., Wood, P. R.·2012·The Astrophysical Journal
DOI 10.1088/0004-637x/746/1/20
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Abstract

We present stellar evolutionary sequences for asymptotic giant branch (AGB) stars in the Magellanic Cloud clusters NGC 1978, NGC 1846, and NGC 419. The new stellar models for the three clusters match the observed effective temperatures on the giant branches, the oxygen-rich to carbon-rich transition luminosities, and the AGB-tip luminosities. A major finding is that a large amount of convective overshoot (up to 3 pressure scale heights) is required at the base of the convective envelope during third dredge-up in order to get the correct oxygen-rich to carbon-rich transition luminosity. The stellar evolution sequences are used as input for detailed nucleosynthesis calculations. For NGC 1978 and NGC 1846 we compare our model results to the observationally derived abundances of carbon and oxygen. We find that additional mixing processes (extra mixing) are required to explain the observed abundance patterns. For NGC 1846 we conclude that non-convective extra mixing processes are required on both the red giant branch and the AGB, in agreement with previous studies. For NGC 1978 it is possible to explain the C/O and 12 C/ 13 C abundances of both the O-rich and the C-rich AGB stars by assuming that the material in the intershell region contains high abundances of both C and O. This may occur during a thermal pulse when convective overshoot at the inner edge of the flash-driven convective pocket dredges C and O from the core to the intershell. For NGC 419 we provide our predicted model abundance values although there are currently no published observed abundance studies for the AGB stars in this cluster.

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Crossref · 10.1088/0004-637x/746/1/20

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  • Deeper mixing alters the predictions of the first dredge-up, but there is a saturation of composition changes such that the small increase needed in the depth of the first dredge-up does not produce an observable difference in the envelope abundances.

    “Of course this deeper mixing alters the predictions of the FDU; however it appears that there is a saturation of composition changes such that the small increase needed in the depth of the FDU does not produce an observable difference in the envelope abundances”

    From The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014) · cites this paper as Kamath et al. 2012

  • The first shell flashes with dredge-up occur for core masses M_min_c ≈ 0.56-0.58 M⊙.

    “The first shell flashes with dredge-up occur for core masses of M min c ≈ 0 . 56 -0 . 58 M ⊙ .”

    From The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014) · cites this paper as Kamath et al. (2012)

  • Such large overshoot leads to λ values in the range 0.66 to 0.82 for the best fitting models.

    “Such large overshoot leads to λ values in the range 0.66 to 0.82 for the best fitting models.”

    From The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014) · cites this paper as Kamath et al. (2012)

  • Kamath et al. (2012) found that a large amount of convective overshoot (up to 3 pressure scale heights) is required at the base of the convective envelope during third dredge-up to get the correct O-rich to C-rich transition luminosity.

    “A major finding from the study by Kamath et al. (2012) is that a large amount of convective overshoot (up to 3 pressure scale heights) is required at the base of the convective envelope during third dredge-up in order to get the correct O-rich to C-rich transition luminosity.”

    From The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014) · cites this paper as Kamath et al. (2012)

  • Observations of F in C-rich AGB stars in the LMC cluster NGC 1846 show a discrepancy with models, with observed F abundance increasing more strongly with C/O ratio than in the theoretical model.

    “Observations of F in the Crich AGB stars in the LMC cluster NGC 1846 however show a discrepancy with models (Lebzelter et al. 2008; Kamath et al. 2012), with the observed F abundance increasing more strongly with the C/O ratio than in the theoretical model.”

    From The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014) · cites this paper as Kamath et al. 2012

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Metadata

Authors
Kamath, D., Karakas, A. I., & Wood, P. R.
Affiliations
Mount Stromlo Observatory (AU)
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2012-01-20
Volume
746
Issue
1
Pages
20
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/746/1/20
OpenAlex
W1797025198
Cited by
55
References
2
Citations by year
2025: 2 · 2023: 2 · 2022: 4 · 2021: 4 · 2020: 3 · 2018: 4 · 2017: 1 · 2016: 5 · 2015: 5 · 2014: 12 · 2013: 9 · 2012: 4
FWCI
5.25
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • ANU Open Research (Australian National University) (submittedVersion)
Funders
National Cancer Institute
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Gamma-ray bursts and supernovae
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords
asymptotic giant branch stars, stellar evolution, nucleosynthesis, NGC 419, convective overshooting, third dredge-up, extra mixing, carbon and oxygen abundances, 13C/12C ratio, thermal pulses, star clusters

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