<sup>17</sup>O Destruction Rate in Stars
In recent years, several laboratory studies of CNO cycle-related nuclear reactions have been carried out. Nevertheless, extant models of stellar nucleosynthesis still adopt CNO reaction rates reported in old compilations, such as NACRE or CF88. In order to update these rates, we performed new calcul...
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2024-10-01
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| author | David Rapagnani Oscar Straniero Gianluca Imbriani |
| author_facet | David Rapagnani Oscar Straniero Gianluca Imbriani |
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| description | In recent years, several laboratory studies of CNO cycle-related nuclear reactions have been carried out. Nevertheless, extant models of stellar nucleosynthesis still adopt CNO reaction rates reported in old compilations, such as NACRE or CF88. In order to update these rates, we performed new calculations based on a Monte Carlo R-Matrix analysis. In more detail, a method was developed that is based on the collection of all the available data, including recent low-energy measurements obtained by the LUNA collaboration in the reduced background environment of the INFN-LNGS underground laboratory, on R-Matrix cross-section calculations with the AZURE2 code and on uncertainty evaluations with a Monte Carlo analysis. As a first scientific benchmark case, the reactions <sup>17</sup>O<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi mathvariant="normal">p</mi><mo>,</mo><mi>γ</mi><mo>)</mo></mrow></semantics></math></inline-formula><sup>18</sup>F and <sup>17</sup>O<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi mathvariant="normal">p</mi><mo>,</mo><mi>α</mi><mo>)</mo></mrow></semantics></math></inline-formula><sup>14</sup>N were investigated. Among the different stellar scenarios they can influence, the <sup>16</sup>O/<sup>17</sup>O abundance ratio in RGB and AGB stars is the one that can be directly confirmed from spectroscopic measurements. The aim is to reduce the nuclear physics uncertainties, thus providing a useful tool to constrain deep mixing processes eventually taking place in these stars. In this work, we present the procedure we followed to calculate the <sup>17</sup>O<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi mathvariant="normal">p</mi><mo>,</mo><mi>γ</mi><mo>)</mo></mrow></semantics></math></inline-formula><sup>18</sup>F and the <sup>17</sup>O<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi mathvariant="normal">p</mi><mo>,</mo><mi>α</mi><mo>)</mo></mrow></semantics></math></inline-formula><sup>14</sup>N reaction stellar rates and preliminary comparisons with similar rates reported in widely used nuclear physics libraries are discussed. |
| format | Article |
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| institution | Kabale University |
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| spelling | doaj-art-e5061fc9cbc94bafb09bdf92a6db8d122024-12-27T14:27:33ZengMDPI AGGalaxies2075-44342024-10-011267110.3390/galaxies12060071<sup>17</sup>O Destruction Rate in StarsDavid Rapagnani0Oscar Straniero1Gianluca Imbriani2Dipartimento di Fisica “E. Pancini”, Università degli Studi di Napoli “Federico II”, Complesso Universitario di Monte Sant’Angelo, Via Cintia, 21, 80125 Naples, ItalyIstituto Nazionale di Astrofisica, Osservatorio Astronomico d’Abruzzo, Via Mentore Maggini, 64100 Teramo, ItalyDipartimento di Fisica “E. Pancini”, Università degli Studi di Napoli “Federico II”, Complesso Universitario di Monte Sant’Angelo, Via Cintia, 21, 80125 Naples, ItalyIn recent years, several laboratory studies of CNO cycle-related nuclear reactions have been carried out. Nevertheless, extant models of stellar nucleosynthesis still adopt CNO reaction rates reported in old compilations, such as NACRE or CF88. In order to update these rates, we performed new calculations based on a Monte Carlo R-Matrix analysis. In more detail, a method was developed that is based on the collection of all the available data, including recent low-energy measurements obtained by the LUNA collaboration in the reduced background environment of the INFN-LNGS underground laboratory, on R-Matrix cross-section calculations with the AZURE2 code and on uncertainty evaluations with a Monte Carlo analysis. As a first scientific benchmark case, the reactions <sup>17</sup>O<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi mathvariant="normal">p</mi><mo>,</mo><mi>γ</mi><mo>)</mo></mrow></semantics></math></inline-formula><sup>18</sup>F and <sup>17</sup>O<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi mathvariant="normal">p</mi><mo>,</mo><mi>α</mi><mo>)</mo></mrow></semantics></math></inline-formula><sup>14</sup>N were investigated. Among the different stellar scenarios they can influence, the <sup>16</sup>O/<sup>17</sup>O abundance ratio in RGB and AGB stars is the one that can be directly confirmed from spectroscopic measurements. The aim is to reduce the nuclear physics uncertainties, thus providing a useful tool to constrain deep mixing processes eventually taking place in these stars. In this work, we present the procedure we followed to calculate the <sup>17</sup>O<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi mathvariant="normal">p</mi><mo>,</mo><mi>γ</mi><mo>)</mo></mrow></semantics></math></inline-formula><sup>18</sup>F and the <sup>17</sup>O<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi mathvariant="normal">p</mi><mo>,</mo><mi>α</mi><mo>)</mo></mrow></semantics></math></inline-formula><sup>14</sup>N reaction stellar rates and preliminary comparisons with similar rates reported in widely used nuclear physics libraries are discussed.https://www.mdpi.com/2075-4434/12/6/71nuclear astrophysicsstellar reaction ratesR-MatrixMonte Carlo analysis |
| spellingShingle | David Rapagnani Oscar Straniero Gianluca Imbriani <sup>17</sup>O Destruction Rate in Stars Galaxies nuclear astrophysics stellar reaction rates R-Matrix Monte Carlo analysis |
| title | <sup>17</sup>O Destruction Rate in Stars |
| title_full | <sup>17</sup>O Destruction Rate in Stars |
| title_fullStr | <sup>17</sup>O Destruction Rate in Stars |
| title_full_unstemmed | <sup>17</sup>O Destruction Rate in Stars |
| title_short | <sup>17</sup>O Destruction Rate in Stars |
| title_sort | sup 17 sup o destruction rate in stars |
| topic | nuclear astrophysics stellar reaction rates R-Matrix Monte Carlo analysis |
| url | https://www.mdpi.com/2075-4434/12/6/71 |
| work_keys_str_mv | AT davidrapagnani sup17supodestructionrateinstars AT oscarstraniero sup17supodestructionrateinstars AT gianlucaimbriani sup17supodestructionrateinstars |