Stellar <i>β</i><sup>−</sup> Decay Rates for <sup>63</sup>Co and <sup>63</sup>Ni by the Projected Shell Model
<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay for <inline-formula><math xmln...
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| Format: | Article |
| Language: | English |
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MDPI AG
2023-01-01
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| Series: | Symmetry |
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| Online Access: | https://www.mdpi.com/2073-8994/15/2/315 |
| _version_ | 1797618096328933376 |
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| author | Zi-Rui Chen Long-Jun Wang |
| author_facet | Zi-Rui Chen Long-Jun Wang |
| author_sort | Zi-Rui Chen |
| collection | DOAJ |
| description | <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay for <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co-<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni-<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Cu region nuclei play important roles in core-collapse supernovae and the slow neutron-capture (<i>s</i>) process. In this work, the stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates for <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni are studied within the projected shell model where the effects of thermally populated parent-nucleus excited states are analyzed. For <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co, the calculated stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates are lower than the results of the conventional shell model. For the <i>s</i>-process branching point <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni, the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rate under a terrestrial condition is well described, and the calculated stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates in the <i>s</i>-process condition turn out to increase with stellar temperature due to the contribution from parent-nucleus excited states. |
| first_indexed | 2024-03-11T08:05:20Z |
| format | Article |
| id | doaj.art-ec3715924ff84f6e848a10218fbf3595 |
| institution | Directory Open Access Journal |
| issn | 2073-8994 |
| language | English |
| last_indexed | 2024-03-11T08:05:20Z |
| publishDate | 2023-01-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Symmetry |
| spelling | doaj.art-ec3715924ff84f6e848a10218fbf35952023-11-16T23:31:41ZengMDPI AGSymmetry2073-89942023-01-0115231510.3390/sym15020315Stellar <i>β</i><sup>−</sup> Decay Rates for <sup>63</sup>Co and <sup>63</sup>Ni by the Projected Shell ModelZi-Rui Chen0Long-Jun Wang1School of Physical Science and Technology, Southwest University, Chongqing 400715, ChinaSchool of Physical Science and Technology, Southwest University, Chongqing 400715, China<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay for <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co-<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni-<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Cu region nuclei play important roles in core-collapse supernovae and the slow neutron-capture (<i>s</i>) process. In this work, the stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates for <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni are studied within the projected shell model where the effects of thermally populated parent-nucleus excited states are analyzed. For <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co, the calculated stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates are lower than the results of the conventional shell model. For the <i>s</i>-process branching point <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni, the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rate under a terrestrial condition is well described, and the calculated stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates in the <i>s</i>-process condition turn out to increase with stellar temperature due to the contribution from parent-nucleus excited states.https://www.mdpi.com/2073-8994/15/2/315<i>β</i><sup>−</sup> decay<i>s</i>-processbranching pointcore-collapse supernovaprojected shell model |
| spellingShingle | Zi-Rui Chen Long-Jun Wang Stellar <i>β</i><sup>−</sup> Decay Rates for <sup>63</sup>Co and <sup>63</sup>Ni by the Projected Shell Model Symmetry <i>β</i><sup>−</sup> decay <i>s</i>-process branching point core-collapse supernova projected shell model |
| title | Stellar <i>β</i><sup>−</sup> Decay Rates for <sup>63</sup>Co and <sup>63</sup>Ni by the Projected Shell Model |
| title_full | Stellar <i>β</i><sup>−</sup> Decay Rates for <sup>63</sup>Co and <sup>63</sup>Ni by the Projected Shell Model |
| title_fullStr | Stellar <i>β</i><sup>−</sup> Decay Rates for <sup>63</sup>Co and <sup>63</sup>Ni by the Projected Shell Model |
| title_full_unstemmed | Stellar <i>β</i><sup>−</sup> Decay Rates for <sup>63</sup>Co and <sup>63</sup>Ni by the Projected Shell Model |
| title_short | Stellar <i>β</i><sup>−</sup> Decay Rates for <sup>63</sup>Co and <sup>63</sup>Ni by the Projected Shell Model |
| title_sort | stellar i β i sup sup decay rates for sup 63 sup co and sup 63 sup ni by the projected shell model |
| topic | <i>β</i><sup>−</sup> decay <i>s</i>-process branching point core-collapse supernova projected shell model |
| url | https://www.mdpi.com/2073-8994/15/2/315 |
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