Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies
Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiment...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Eroğlu, M. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2023 |
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| Anmerkung: |
© The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. |
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| Übergeordnetes Werk: |
Enthalten in: Nuclear science and techniques - Singapore : Springer, 2006, 34(2023), 11 vom: Nov. |
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| Übergeordnetes Werk: |
volume:34 ; year:2023 ; number:11 ; month:11 |
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| DOI / URN: |
10.1007/s41365-023-01301-4 |
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| Katalog-ID: |
SPR053744365 |
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| 245 | 1 | 0 | |a Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies |
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| 520 | |a Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. | ||
| 650 | 4 | |a Cross section |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Astrophysical S-factor |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Astrophysical reaction rate |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a p-process nucleosynthesis |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Threshold logic unit method |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Yalçın, C. |0 (orcid)0000-0002-3105-7267 |4 aut | |
| 700 | 1 | |a Güray, R. T. |0 (orcid)0000-0002-5481-9981 |4 aut | |
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10.1007/s41365-023-01301-4 doi (DE-627)SPR053744365 (SPR)s41365-023-01301-4-e DE-627 ger DE-627 rakwb eng Eroğlu, M. verfasserin (orcid)0000-0003-4220-1356 aut Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. Cross section (dpeaa)DE-He213 Astrophysical S-factor (dpeaa)DE-He213 Astrophysical reaction rate (dpeaa)DE-He213 p-process nucleosynthesis (dpeaa)DE-He213 Threshold logic unit method (dpeaa)DE-He213 Yalçın, C. (orcid)0000-0002-3105-7267 aut Güray, R. T. (orcid)0000-0002-5481-9981 aut Enthalten in Nuclear science and techniques Singapore : Springer, 2006 34(2023), 11 vom: Nov. (DE-627)513219439 (DE-600)2238719-5 2210-3147 nnns volume:34 year:2023 number:11 month:11 https://dx.doi.org/10.1007/s41365-023-01301-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 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_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 34 2023 11 11 |
| spelling |
10.1007/s41365-023-01301-4 doi (DE-627)SPR053744365 (SPR)s41365-023-01301-4-e DE-627 ger DE-627 rakwb eng Eroğlu, M. verfasserin (orcid)0000-0003-4220-1356 aut Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. Cross section (dpeaa)DE-He213 Astrophysical S-factor (dpeaa)DE-He213 Astrophysical reaction rate (dpeaa)DE-He213 p-process nucleosynthesis (dpeaa)DE-He213 Threshold logic unit method (dpeaa)DE-He213 Yalçın, C. (orcid)0000-0002-3105-7267 aut Güray, R. T. (orcid)0000-0002-5481-9981 aut Enthalten in Nuclear science and techniques Singapore : Springer, 2006 34(2023), 11 vom: Nov. (DE-627)513219439 (DE-600)2238719-5 2210-3147 nnns volume:34 year:2023 number:11 month:11 https://dx.doi.org/10.1007/s41365-023-01301-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 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_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 34 2023 11 11 |
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10.1007/s41365-023-01301-4 doi (DE-627)SPR053744365 (SPR)s41365-023-01301-4-e DE-627 ger DE-627 rakwb eng Eroğlu, M. verfasserin (orcid)0000-0003-4220-1356 aut Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. Cross section (dpeaa)DE-He213 Astrophysical S-factor (dpeaa)DE-He213 Astrophysical reaction rate (dpeaa)DE-He213 p-process nucleosynthesis (dpeaa)DE-He213 Threshold logic unit method (dpeaa)DE-He213 Yalçın, C. (orcid)0000-0002-3105-7267 aut Güray, R. T. (orcid)0000-0002-5481-9981 aut Enthalten in Nuclear science and techniques Singapore : Springer, 2006 34(2023), 11 vom: Nov. (DE-627)513219439 (DE-600)2238719-5 2210-3147 nnns volume:34 year:2023 number:11 month:11 https://dx.doi.org/10.1007/s41365-023-01301-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 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_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 34 2023 11 11 |
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10.1007/s41365-023-01301-4 doi (DE-627)SPR053744365 (SPR)s41365-023-01301-4-e DE-627 ger DE-627 rakwb eng Eroğlu, M. verfasserin (orcid)0000-0003-4220-1356 aut Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. Cross section (dpeaa)DE-He213 Astrophysical S-factor (dpeaa)DE-He213 Astrophysical reaction rate (dpeaa)DE-He213 p-process nucleosynthesis (dpeaa)DE-He213 Threshold logic unit method (dpeaa)DE-He213 Yalçın, C. (orcid)0000-0002-3105-7267 aut Güray, R. T. (orcid)0000-0002-5481-9981 aut Enthalten in Nuclear science and techniques Singapore : Springer, 2006 34(2023), 11 vom: Nov. (DE-627)513219439 (DE-600)2238719-5 2210-3147 nnns volume:34 year:2023 number:11 month:11 https://dx.doi.org/10.1007/s41365-023-01301-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 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_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 34 2023 11 11 |
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10.1007/s41365-023-01301-4 doi (DE-627)SPR053744365 (SPR)s41365-023-01301-4-e DE-627 ger DE-627 rakwb eng Eroğlu, M. verfasserin (orcid)0000-0003-4220-1356 aut Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. Cross section (dpeaa)DE-He213 Astrophysical S-factor (dpeaa)DE-He213 Astrophysical reaction rate (dpeaa)DE-He213 p-process nucleosynthesis (dpeaa)DE-He213 Threshold logic unit method (dpeaa)DE-He213 Yalçın, C. (orcid)0000-0002-3105-7267 aut Güray, R. T. (orcid)0000-0002-5481-9981 aut Enthalten in Nuclear science and techniques Singapore : Springer, 2006 34(2023), 11 vom: Nov. (DE-627)513219439 (DE-600)2238719-5 2210-3147 nnns volume:34 year:2023 number:11 month:11 https://dx.doi.org/10.1007/s41365-023-01301-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 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_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 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_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 34 2023 11 11 |
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(Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law.</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. 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Eroğlu, M. |
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Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies Cross section (dpeaa)DE-He213 Astrophysical S-factor (dpeaa)DE-He213 Astrophysical reaction rate (dpeaa)DE-He213 p-process nucleosynthesis (dpeaa)DE-He213 Threshold logic unit method (dpeaa)DE-He213 |
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investigation of the 121sb(α,γ)125i reaction cross-section calculations at astrophysical energies |
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Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies |
| abstract |
Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. © The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. |
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Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. © The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. |
| abstract_unstemmed |
Abstract Proton-rich nuclei are synthesized via photodisintegration and reverse reactions. To examine this mechanism and reproduce the observed p-nucleus abundances, it is crucial to know the reaction rates and thereby the reaction cross sections of many isotopes. Given that the number of experiments on the reactions in astrophysical energy regions is very rare, the reaction cross sections are determined by theoretical methods whose accuracy should be tested. In this study, given that %$^{121}%$Sb is a stable seed isotope located in the region of medium-mass p-nuclei, we investigated the cross sections and reaction rates of the %$^{121}%$Sb(%$\alpha%$,%$\gamma%$)%$^{125}%$I reaction using the TALYS computer code with 432 different combinations of input parameters (OMP, LDM, and SFM). The optimal model combinations were determined using the threshold logic unit method. The theoretical reaction cross-sectional results were compared with the experimental results reported in the literature. The reaction rates were determined using the two input parameter sets most compatible with the measurements, and they were compared with the reaction rate databases: STARLIB and REACLIB. © The Author(s), under exclusive licence to China Science Publishing & Media Ltd. (Science Press), Shanghai Institute of Applied Physics, the Chinese Academy of Sciences, Chinese Nuclear Society 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law. |
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11 |
| title_short |
Investigation of the 121Sb(α,γ)125I reaction cross-section calculations at astrophysical energies |
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https://dx.doi.org/10.1007/s41365-023-01301-4 |
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Yalçın, C. Güray, R. T. |
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Yalçın, C. Güray, R. T. |
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10.1007/s41365-023-01301-4 |
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2024-07-03T21:43:18.303Z |
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| score |
7.402338 |