First inverse kinematics measurement of key resonances in the
In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Lennarz, A. [verfasserIn] Williams, M. [verfasserIn] Laird, A.M. [verfasserIn] Battino, U. [verfasserIn] Chen, A.A. [verfasserIn] Connolly, D. [verfasserIn] Davids, B. [verfasserIn] Esker, N. [verfasserIn] Garg, R. [verfasserIn] Gay, M. [verfasserIn] Greife, U. [verfasserIn] Hager, U. [verfasserIn] Hutcheon, D. [verfasserIn] José, J. [verfasserIn] Lovely, M. [verfasserIn] Lyons, S. [verfasserIn] Psaltis, A. [verfasserIn] Riley, J.E. [verfasserIn] Tattersall, A. [verfasserIn] Ruiz, C. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2020 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Physics letters - Amsterdam : North-Holland Publ, 2011, 807 |
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| Übergeordnetes Werk: |
volume:807 |
| DOI / URN: |
10.1016/j.physletb.2020.135539 |
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| Katalog-ID: |
ELV004507169 |
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| 245 | 1 | 0 | |a First inverse kinematics measurement of key resonances in the |
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| 520 | |a In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. | ||
| 650 | 4 | |a Inverse kinematics measurements | |
| 650 | 4 | |a Radiative capture reactions | |
| 650 | 4 | |a Stellar nucleosynthesis | |
| 700 | 1 | |a Williams, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Laird, A.M. |e verfasserin |4 aut | |
| 700 | 1 | |a Battino, U. |e verfasserin |0 (orcid)0000-0002-4619-8492 |4 aut | |
| 700 | 1 | |a Chen, A.A. |e verfasserin |0 (orcid)0000-0001-6515-6266 |4 aut | |
| 700 | 1 | |a Connolly, D. |e verfasserin |0 (orcid)0000-0001-9104-7485 |4 aut | |
| 700 | 1 | |a Davids, B. |e verfasserin |4 aut | |
| 700 | 1 | |a Esker, N. |e verfasserin |0 (orcid)0000-0002-5381-4927 |4 aut | |
| 700 | 1 | |a Garg, R. |e verfasserin |4 aut | |
| 700 | 1 | |a Gay, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Greife, U. |e verfasserin |4 aut | |
| 700 | 1 | |a Hager, U. |e verfasserin |4 aut | |
| 700 | 1 | |a Hutcheon, D. |e verfasserin |4 aut | |
| 700 | 1 | |a José, J. |e verfasserin |0 (orcid)0000-0002-9937-2685 |4 aut | |
| 700 | 1 | |a Lovely, M. |e verfasserin |0 (orcid)0000-0002-4067-9025 |4 aut | |
| 700 | 1 | |a Lyons, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Psaltis, A. |e verfasserin |4 aut | |
| 700 | 1 | |a Riley, J.E. |e verfasserin |0 (orcid)0000-0001-8617-1422 |4 aut | |
| 700 | 1 | |a Tattersall, A. |e verfasserin |0 (orcid)0000-0001-7958-6590 |4 aut | |
| 700 | 1 | |a Ruiz, C. |e verfasserin |4 aut | |
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10.1016/j.physletb.2020.135539 doi (DE-627)ELV004507169 (ELSEVIER)S0370-2693(20)30343-9 DE-627 ger DE-627 rda eng 530 VZ Lennarz, A. verfasserin (orcid)0000-0002-8138-0126 aut First inverse kinematics measurement of key resonances in the 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. Inverse kinematics measurements Radiative capture reactions Stellar nucleosynthesis Williams, M. verfasserin aut Laird, A.M. verfasserin aut Battino, U. verfasserin (orcid)0000-0002-4619-8492 aut Chen, A.A. verfasserin (orcid)0000-0001-6515-6266 aut Connolly, D. verfasserin (orcid)0000-0001-9104-7485 aut Davids, B. verfasserin aut Esker, N. verfasserin (orcid)0000-0002-5381-4927 aut Garg, R. verfasserin aut Gay, M. verfasserin aut Greife, U. verfasserin aut Hager, U. verfasserin aut Hutcheon, D. verfasserin aut José, J. verfasserin (orcid)0000-0002-9937-2685 aut Lovely, M. verfasserin (orcid)0000-0002-4067-9025 aut Lyons, S. verfasserin aut Psaltis, A. verfasserin aut Riley, J.E. verfasserin (orcid)0000-0001-8617-1422 aut Tattersall, A. verfasserin (orcid)0000-0001-7958-6590 aut Ruiz, C. verfasserin aut Enthalten in Physics letters Amsterdam : North-Holland Publ, 2011 807 (DE-627)266015360 (DE-600)1466612-1 nnns volume:807 GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 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 807 |
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10.1016/j.physletb.2020.135539 doi (DE-627)ELV004507169 (ELSEVIER)S0370-2693(20)30343-9 DE-627 ger DE-627 rda eng 530 VZ Lennarz, A. verfasserin (orcid)0000-0002-8138-0126 aut First inverse kinematics measurement of key resonances in the 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. Inverse kinematics measurements Radiative capture reactions Stellar nucleosynthesis Williams, M. verfasserin aut Laird, A.M. verfasserin aut Battino, U. verfasserin (orcid)0000-0002-4619-8492 aut Chen, A.A. verfasserin (orcid)0000-0001-6515-6266 aut Connolly, D. verfasserin (orcid)0000-0001-9104-7485 aut Davids, B. verfasserin aut Esker, N. verfasserin (orcid)0000-0002-5381-4927 aut Garg, R. verfasserin aut Gay, M. verfasserin aut Greife, U. verfasserin aut Hager, U. verfasserin aut Hutcheon, D. verfasserin aut José, J. verfasserin (orcid)0000-0002-9937-2685 aut Lovely, M. verfasserin (orcid)0000-0002-4067-9025 aut Lyons, S. verfasserin aut Psaltis, A. verfasserin aut Riley, J.E. verfasserin (orcid)0000-0001-8617-1422 aut Tattersall, A. verfasserin (orcid)0000-0001-7958-6590 aut Ruiz, C. verfasserin aut Enthalten in Physics letters Amsterdam : North-Holland Publ, 2011 807 (DE-627)266015360 (DE-600)1466612-1 nnns volume:807 GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 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 807 |
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10.1016/j.physletb.2020.135539 doi (DE-627)ELV004507169 (ELSEVIER)S0370-2693(20)30343-9 DE-627 ger DE-627 rda eng 530 VZ Lennarz, A. verfasserin (orcid)0000-0002-8138-0126 aut First inverse kinematics measurement of key resonances in the 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. Inverse kinematics measurements Radiative capture reactions Stellar nucleosynthesis Williams, M. verfasserin aut Laird, A.M. verfasserin aut Battino, U. verfasserin (orcid)0000-0002-4619-8492 aut Chen, A.A. verfasserin (orcid)0000-0001-6515-6266 aut Connolly, D. verfasserin (orcid)0000-0001-9104-7485 aut Davids, B. verfasserin aut Esker, N. verfasserin (orcid)0000-0002-5381-4927 aut Garg, R. verfasserin aut Gay, M. verfasserin aut Greife, U. verfasserin aut Hager, U. verfasserin aut Hutcheon, D. verfasserin aut José, J. verfasserin (orcid)0000-0002-9937-2685 aut Lovely, M. verfasserin (orcid)0000-0002-4067-9025 aut Lyons, S. verfasserin aut Psaltis, A. verfasserin aut Riley, J.E. verfasserin (orcid)0000-0001-8617-1422 aut Tattersall, A. verfasserin (orcid)0000-0001-7958-6590 aut Ruiz, C. verfasserin aut Enthalten in Physics letters Amsterdam : North-Holland Publ, 2011 807 (DE-627)266015360 (DE-600)1466612-1 nnns volume:807 GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 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 807 |
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10.1016/j.physletb.2020.135539 doi (DE-627)ELV004507169 (ELSEVIER)S0370-2693(20)30343-9 DE-627 ger DE-627 rda eng 530 VZ Lennarz, A. verfasserin (orcid)0000-0002-8138-0126 aut First inverse kinematics measurement of key resonances in the 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. Inverse kinematics measurements Radiative capture reactions Stellar nucleosynthesis Williams, M. verfasserin aut Laird, A.M. verfasserin aut Battino, U. verfasserin (orcid)0000-0002-4619-8492 aut Chen, A.A. verfasserin (orcid)0000-0001-6515-6266 aut Connolly, D. verfasserin (orcid)0000-0001-9104-7485 aut Davids, B. verfasserin aut Esker, N. verfasserin (orcid)0000-0002-5381-4927 aut Garg, R. verfasserin aut Gay, M. verfasserin aut Greife, U. verfasserin aut Hager, U. verfasserin aut Hutcheon, D. verfasserin aut José, J. verfasserin (orcid)0000-0002-9937-2685 aut Lovely, M. verfasserin (orcid)0000-0002-4067-9025 aut Lyons, S. verfasserin aut Psaltis, A. verfasserin aut Riley, J.E. verfasserin (orcid)0000-0001-8617-1422 aut Tattersall, A. verfasserin (orcid)0000-0001-7958-6590 aut Ruiz, C. verfasserin aut Enthalten in Physics letters Amsterdam : North-Holland Publ, 2011 807 (DE-627)266015360 (DE-600)1466612-1 nnns volume:807 GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 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 807 |
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10.1016/j.physletb.2020.135539 doi (DE-627)ELV004507169 (ELSEVIER)S0370-2693(20)30343-9 DE-627 ger DE-627 rda eng 530 VZ Lennarz, A. verfasserin (orcid)0000-0002-8138-0126 aut First inverse kinematics measurement of key resonances in the 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. Inverse kinematics measurements Radiative capture reactions Stellar nucleosynthesis Williams, M. verfasserin aut Laird, A.M. verfasserin aut Battino, U. verfasserin (orcid)0000-0002-4619-8492 aut Chen, A.A. verfasserin (orcid)0000-0001-6515-6266 aut Connolly, D. verfasserin (orcid)0000-0001-9104-7485 aut Davids, B. verfasserin aut Esker, N. verfasserin (orcid)0000-0002-5381-4927 aut Garg, R. verfasserin aut Gay, M. verfasserin aut Greife, U. verfasserin aut Hager, U. verfasserin aut Hutcheon, D. verfasserin aut José, J. verfasserin (orcid)0000-0002-9937-2685 aut Lovely, M. verfasserin (orcid)0000-0002-4067-9025 aut Lyons, S. verfasserin aut Psaltis, A. verfasserin aut Riley, J.E. verfasserin (orcid)0000-0001-8617-1422 aut Tattersall, A. verfasserin (orcid)0000-0001-7958-6590 aut Ruiz, C. verfasserin aut Enthalten in Physics letters Amsterdam : North-Holland Publ, 2011 807 (DE-627)266015360 (DE-600)1466612-1 nnns volume:807 GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2014 GBV_ILN_2025 GBV_ILN_2034 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2064 GBV_ILN_2111 GBV_ILN_2153 GBV_ILN_2336 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4251 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 807 |
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Lennarz, A. @@aut@@ Williams, M. @@aut@@ Laird, A.M. @@aut@@ Battino, U. @@aut@@ Chen, A.A. @@aut@@ Connolly, D. @@aut@@ Davids, B. @@aut@@ Esker, N. @@aut@@ Garg, R. @@aut@@ Gay, M. @@aut@@ Greife, U. @@aut@@ Hager, U. @@aut@@ Hutcheon, D. @@aut@@ José, J. @@aut@@ Lovely, M. @@aut@@ Lyons, S. @@aut@@ Psaltis, A. @@aut@@ Riley, J.E. @@aut@@ Tattersall, A. @@aut@@ Ruiz, C. @@aut@@ |
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Lennarz, A. Williams, M. Laird, A.M. Battino, U. Chen, A.A. Connolly, D. Davids, B. Esker, N. Garg, R. Gay, M. Greife, U. Hager, U. Hutcheon, D. José, J. Lovely, M. Lyons, S. Psaltis, A. Riley, J.E. Tattersall, A. Ruiz, C. |
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first inverse kinematics measurement of key resonances in the |
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First inverse kinematics measurement of key resonances in the |
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In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. |
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In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. |
| abstract_unstemmed |
In this Letter we report on the first inverse kinematics measurement of key resonances in the Ne 22 ( p , γ ) 23 Na reaction which forms part of the NeNa cycle, and is relevant for 23Na synthesis in asymptotic giant branch (AGB) stars. An anti-correlation in O and Na abundances is seen across all well-studied globular clusters (GC), however, reaction-rate uncertainties limit the precision as to which stellar evolution models can reproduce the observed isotopic abundance patterns. Given the importance of GC observations in testing stellar evolution models and their dependence on NeNa reaction rates, it is critical that the nuclear physics uncertainties on the origin of 23Na be addressed. We present results of direct strengths measurements of four key resonances in Ne 22 ( p , γ ) 23 Na at E c . m . = 149 keV, 181 keV, 248 keV and 458 keV. The strength of the important E c . m . = 458 keV reference resonance has been determined independently of other resonance strengths for the first time with an associated strength of ωγ = 0.439(22) eV and with higher precision than previously reported. Our result deviates from the two most recently published results obtained from normal kinematics measurements performed by the LENA and LUNA collaborations but is in agreement with earlier measurements. The impact of our rate on the Na-pocket formation in AGB stars and its relation to the O-Na anti-correlation was assessed via network calculations. Further, the effect on isotopic abundances in CO and ONe novae ejecta with respect to pre-solar grains was investigated. |
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First inverse kinematics measurement of key resonances in the |
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| score |
7.399908 |