New 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-process
Accurate nuclear reaction rates for ^26 P( p , γ ) ^27 S are pivotal for a comprehensive understanding of the rp -process nucleosynthesis path in the region of proton-rich sulfur and phosphorus isotopes. However, large uncertainties still exist in the current rate of ^26 P( p , γ ) ^27 S because of...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/accf9c |
| _version_ | 1827826110810816512 |
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| author | S. Q. Hou J. B. Liu T. C. L. Trueman J. G. Li M. Pignatari C. A. Bertulani X. X. Xu |
| author_facet | S. Q. Hou J. B. Liu T. C. L. Trueman J. G. Li M. Pignatari C. A. Bertulani X. X. Xu |
| author_sort | S. Q. Hou |
| collection | DOAJ |
| description | Accurate nuclear reaction rates for ^26 P( p , γ ) ^27 S are pivotal for a comprehensive understanding of the rp -process nucleosynthesis path in the region of proton-rich sulfur and phosphorus isotopes. However, large uncertainties still exist in the current rate of ^26 P( p , γ ) ^27 S because of the lack of nuclear mass and energy level structure information for ^27 S. We reevaluate this reaction rate using the experimentally constrained ^27 S mass, together with the shell model predicted level structure. It is found that the ^26 P( p , γ ) ^27 S reaction rate is dominated by a direct capture reaction mechanism despite the presence of three resonances at E = 1.104, 1.597, and 1.777 MeV above the proton threshold in ^27 S. The new rate is overall smaller than the other previous rates from the Hauser–Feshbach statistical model by at least 1 order of magnitude in the temperature range of X-ray burst interest. In addition, we consistently update the photodisintegration rate using the new ^27 S mass. The influence of new rates of forward and reverse reaction in the abundances of isotopes produced in the rp -process is explored by postprocessing nucleosynthesis calculations. The final abundance ratio of ^27 S/ ^26 P obtained using the new rates is only 10% of that from the old rate. The abundance flow calculations show that the reaction path ^26 P( p , γ ) ^27 S( β ^+ , ν ) ^27 P is not as important as previously thought for producing ^27 P. The adoption of the new reaction rates for ^26 P( p , γ ) ^27 S only reduces the final production of aluminum by 7.1% and has no discernible impact on the yield of other elements. |
| first_indexed | 2024-03-12T03:00:04Z |
| format | Article |
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| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:00:04Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-55968537c84b4742b4684add0874b44e2023-09-03T14:49:40ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01950213310.3847/1538-4357/accf9cNew 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-processS. Q. Hou0https://orcid.org/0000-0001-9182-0853J. B. Liu1T. C. L. Trueman2J. G. Li3M. Pignatari4https://orcid.org/0000-0002-9048-6010C. A. Bertulani5https://orcid.org/0000-0002-4065-6237X. X. Xu6CAS Key Laboratory of High Precision Nuclear Spectroscopy, Institute of Modern Physics , Chinese Academy of Sciences, Lanzhou 730000, People's Republic of China ; sqhou@impcas.ac.cn; School of Nuclear Science and Technology, University of Chinese Academy of Sciences , Beijing 100049, People's Republic of ChinaCAS Key Laboratory of High Precision Nuclear Spectroscopy, Institute of Modern Physics , Chinese Academy of Sciences, Lanzhou 730000, People's Republic of China ; sqhou@impcas.ac.cn; School of Nuclear Science and Technology, University of Chinese Academy of Sciences , Beijing 100049, People's Republic of ChinaKonkoly Observatory, Research Centre for Astronomy and Earth Sciences , Hungarian Academy of Sciences, H-1121 Budapest, Hungary; CSFK, MTA Centre of Excellence, H-1121 Budapest, Hungary; E.A. Milne Centre for Astrophysics, University of Hull, Kingston upon Hull HU6 7RX, UKCAS Key Laboratory of High Precision Nuclear Spectroscopy, Institute of Modern Physics , Chinese Academy of Sciences, Lanzhou 730000, People's Republic of China ; sqhou@impcas.ac.cn; School of Nuclear Science and Technology, University of Chinese Academy of Sciences , Beijing 100049, People's Republic of ChinaKonkoly Observatory, Research Centre for Astronomy and Earth Sciences , Hungarian Academy of Sciences, H-1121 Budapest, Hungary; CSFK, MTA Centre of Excellence, H-1121 Budapest, Hungary; E.A. Milne Centre for Astrophysics, University of Hull, Kingston upon Hull HU6 7RX, UK; Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USADepartment of Physics and Astronomy, Texas A&M University–Commerce , Commerce, TX 75429, USACAS Key Laboratory of High Precision Nuclear Spectroscopy, Institute of Modern Physics , Chinese Academy of Sciences, Lanzhou 730000, People's Republic of China ; sqhou@impcas.ac.cn; School of Nuclear Science and Technology, University of Chinese Academy of Sciences , Beijing 100049, People's Republic of ChinaAccurate nuclear reaction rates for ^26 P( p , γ ) ^27 S are pivotal for a comprehensive understanding of the rp -process nucleosynthesis path in the region of proton-rich sulfur and phosphorus isotopes. However, large uncertainties still exist in the current rate of ^26 P( p , γ ) ^27 S because of the lack of nuclear mass and energy level structure information for ^27 S. We reevaluate this reaction rate using the experimentally constrained ^27 S mass, together with the shell model predicted level structure. It is found that the ^26 P( p , γ ) ^27 S reaction rate is dominated by a direct capture reaction mechanism despite the presence of three resonances at E = 1.104, 1.597, and 1.777 MeV above the proton threshold in ^27 S. The new rate is overall smaller than the other previous rates from the Hauser–Feshbach statistical model by at least 1 order of magnitude in the temperature range of X-ray burst interest. In addition, we consistently update the photodisintegration rate using the new ^27 S mass. The influence of new rates of forward and reverse reaction in the abundances of isotopes produced in the rp -process is explored by postprocessing nucleosynthesis calculations. The final abundance ratio of ^27 S/ ^26 P obtained using the new rates is only 10% of that from the old rate. The abundance flow calculations show that the reaction path ^26 P( p , γ ) ^27 S( β ^+ , ν ) ^27 P is not as important as previously thought for producing ^27 P. The adoption of the new reaction rates for ^26 P( p , γ ) ^27 S only reduces the final production of aluminum by 7.1% and has no discernible impact on the yield of other elements.https://doi.org/10.3847/1538-4357/accf9cReaction ratesX-ray burstsNuclear physicsNuclear abundancesExplosive nucleosynthesis |
| spellingShingle | S. Q. Hou J. B. Liu T. C. L. Trueman J. G. Li M. Pignatari C. A. Bertulani X. X. Xu New 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-process The Astrophysical Journal Reaction rates X-ray bursts Nuclear physics Nuclear abundances Explosive nucleosynthesis |
| title | New 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-process |
| title_full | New 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-process |
| title_fullStr | New 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-process |
| title_full_unstemmed | New 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-process |
| title_short | New 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-process |
| title_sort | new 26p p γ 27s thermonuclear reaction rate and its astrophysical implications in the rp process |
| topic | Reaction rates X-ray bursts Nuclear physics Nuclear abundances Explosive nucleosynthesis |
| url | https://doi.org/10.3847/1538-4357/accf9c |
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