Evidence of Third Dredge-up in Post-AGB Stars in Galactic Globular Clusters
To better understand the mixing and mass loss experienced by low-mass stars as they ascend the asymptotic giant branch (AGB), I have gathered from the literature the abundances of CNO and s -process elements in post-AGB stars in Galactic globular clusters. These species are mixed to the surface duri...
Ausführliche Beschreibung
Autor*in: |
William V. Dixon [verfasserIn] |
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Format: |
E-Artikel |
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Sprache: |
Englisch |
Erschienen: |
2024 |
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Schlagwörter: |
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Übergeordnetes Werk: |
In: The Astrophysical Journal - IOP Publishing, 2022, 961(2024), 1, p 24 |
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Übergeordnetes Werk: |
volume:961 ; year:2024 ; number:1, p 24 |
Links: |
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DOI / URN: |
10.3847/1538-4357/ad0a89 |
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Katalog-ID: |
DOAJ097737585 |
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520 | |a To better understand the mixing and mass loss experienced by low-mass stars as they ascend the asymptotic giant branch (AGB), I have gathered from the literature the abundances of CNO and s -process elements in post-AGB stars in Galactic globular clusters. These species are mixed to the surface during third dredge-up (3DU) events, so their abundance should increase as the star ascends the AGB. Of the 17 stars in this sample, CNO abundances are available for 11. Of these, four are enhanced in CNO relative to the red giant branch stars from which they descended, which I take as evidence of 3DU on the AGB. The enhancement is mainly in the form of carbon. Of the six stars for which only heavy-element abundances are available, one shows s -process enhancements that previous authors have interpreted as evidence of 3DU. Combining these 17 stars with other recent samples reveals that most globular-cluster post-AGB stars have luminosities $\mathrm{log}(L/{L}_{\odot })\sim 3.25$ . They are the progeny of blue horizontal-branch (HB) stars in clusters with intermediate metallicity ([Fe/H] ∼ −1.5). A second group consists of sub-luminous stars associated with high-metallicity clusters ([Fe/H] ∼ −1.0) with red HBs. They may be burning helium, rather than hydrogen. A third group of hot, super-luminous stars is evolving quickly across the Hertzsprung–Russell diagram. Some of them may be merger remnants. | ||
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10.3847/1538-4357/ad0a89 doi (DE-627)DOAJ097737585 (DE-599)DOAJ26a14544f5b143d3957ac6ad652593ca DE-627 ger DE-627 rakwb eng QB460-466 William V. Dixon verfasserin aut Evidence of Third Dredge-up in Post-AGB Stars in Galactic Globular Clusters 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier To better understand the mixing and mass loss experienced by low-mass stars as they ascend the asymptotic giant branch (AGB), I have gathered from the literature the abundances of CNO and s -process elements in post-AGB stars in Galactic globular clusters. These species are mixed to the surface during third dredge-up (3DU) events, so their abundance should increase as the star ascends the AGB. Of the 17 stars in this sample, CNO abundances are available for 11. Of these, four are enhanced in CNO relative to the red giant branch stars from which they descended, which I take as evidence of 3DU on the AGB. The enhancement is mainly in the form of carbon. Of the six stars for which only heavy-element abundances are available, one shows s -process enhancements that previous authors have interpreted as evidence of 3DU. Combining these 17 stars with other recent samples reveals that most globular-cluster post-AGB stars have luminosities $\mathrm{log}(L/{L}_{\odot })\sim 3.25$ . They are the progeny of blue horizontal-branch (HB) stars in clusters with intermediate metallicity ([Fe/H] ∼ −1.5). A second group consists of sub-luminous stars associated with high-metallicity clusters ([Fe/H] ∼ −1.0) with red HBs. They may be burning helium, rather than hydrogen. A third group of hot, super-luminous stars is evolving quickly across the Hertzsprung–Russell diagram. Some of them may be merger remnants. Stellar abundances Asymptotic giant branch stars Post-asymptotic giant branch stars Stellar atmospheres Astrophysics In The Astrophysical Journal IOP Publishing, 2022 961(2024), 1, p 24 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:961 year:2024 number:1, p 24 https://doi.org/10.3847/1538-4357/ad0a89 kostenfrei https://doaj.org/article/26a14544f5b143d3957ac6ad652593ca kostenfrei https://doi.org/10.3847/1538-4357/ad0a89 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 961 2024 1, p 24 |
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William V. Dixon |
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William V. Dixon misc QB460-466 misc Stellar abundances misc Asymptotic giant branch stars misc Post-asymptotic giant branch stars misc Stellar atmospheres misc Astrophysics Evidence of Third Dredge-up in Post-AGB Stars in Galactic Globular Clusters |
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QB460-466 Evidence of Third Dredge-up in Post-AGB Stars in Galactic Globular Clusters Stellar abundances Asymptotic giant branch stars Post-asymptotic giant branch stars Stellar atmospheres |
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evidence of third dredge-up in post-agb stars in galactic globular clusters |
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Evidence of Third Dredge-up in Post-AGB Stars in Galactic Globular Clusters |
abstract |
To better understand the mixing and mass loss experienced by low-mass stars as they ascend the asymptotic giant branch (AGB), I have gathered from the literature the abundances of CNO and s -process elements in post-AGB stars in Galactic globular clusters. These species are mixed to the surface during third dredge-up (3DU) events, so their abundance should increase as the star ascends the AGB. Of the 17 stars in this sample, CNO abundances are available for 11. Of these, four are enhanced in CNO relative to the red giant branch stars from which they descended, which I take as evidence of 3DU on the AGB. The enhancement is mainly in the form of carbon. Of the six stars for which only heavy-element abundances are available, one shows s -process enhancements that previous authors have interpreted as evidence of 3DU. Combining these 17 stars with other recent samples reveals that most globular-cluster post-AGB stars have luminosities $\mathrm{log}(L/{L}_{\odot })\sim 3.25$ . They are the progeny of blue horizontal-branch (HB) stars in clusters with intermediate metallicity ([Fe/H] ∼ −1.5). A second group consists of sub-luminous stars associated with high-metallicity clusters ([Fe/H] ∼ −1.0) with red HBs. They may be burning helium, rather than hydrogen. A third group of hot, super-luminous stars is evolving quickly across the Hertzsprung–Russell diagram. Some of them may be merger remnants. |
abstractGer |
To better understand the mixing and mass loss experienced by low-mass stars as they ascend the asymptotic giant branch (AGB), I have gathered from the literature the abundances of CNO and s -process elements in post-AGB stars in Galactic globular clusters. These species are mixed to the surface during third dredge-up (3DU) events, so their abundance should increase as the star ascends the AGB. Of the 17 stars in this sample, CNO abundances are available for 11. Of these, four are enhanced in CNO relative to the red giant branch stars from which they descended, which I take as evidence of 3DU on the AGB. The enhancement is mainly in the form of carbon. Of the six stars for which only heavy-element abundances are available, one shows s -process enhancements that previous authors have interpreted as evidence of 3DU. Combining these 17 stars with other recent samples reveals that most globular-cluster post-AGB stars have luminosities $\mathrm{log}(L/{L}_{\odot })\sim 3.25$ . They are the progeny of blue horizontal-branch (HB) stars in clusters with intermediate metallicity ([Fe/H] ∼ −1.5). A second group consists of sub-luminous stars associated with high-metallicity clusters ([Fe/H] ∼ −1.0) with red HBs. They may be burning helium, rather than hydrogen. A third group of hot, super-luminous stars is evolving quickly across the Hertzsprung–Russell diagram. Some of them may be merger remnants. |
abstract_unstemmed |
To better understand the mixing and mass loss experienced by low-mass stars as they ascend the asymptotic giant branch (AGB), I have gathered from the literature the abundances of CNO and s -process elements in post-AGB stars in Galactic globular clusters. These species are mixed to the surface during third dredge-up (3DU) events, so their abundance should increase as the star ascends the AGB. Of the 17 stars in this sample, CNO abundances are available for 11. Of these, four are enhanced in CNO relative to the red giant branch stars from which they descended, which I take as evidence of 3DU on the AGB. The enhancement is mainly in the form of carbon. Of the six stars for which only heavy-element abundances are available, one shows s -process enhancements that previous authors have interpreted as evidence of 3DU. Combining these 17 stars with other recent samples reveals that most globular-cluster post-AGB stars have luminosities $\mathrm{log}(L/{L}_{\odot })\sim 3.25$ . They are the progeny of blue horizontal-branch (HB) stars in clusters with intermediate metallicity ([Fe/H] ∼ −1.5). A second group consists of sub-luminous stars associated with high-metallicity clusters ([Fe/H] ∼ −1.0) with red HBs. They may be burning helium, rather than hydrogen. A third group of hot, super-luminous stars is evolving quickly across the Hertzsprung–Russell diagram. Some of them may be merger remnants. |
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Evidence of Third Dredge-up in Post-AGB Stars in Galactic Globular Clusters |
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