Neutrino cooling rates due to nickel isotopes for presupernova evolution of massive stars
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arXiv
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| Autori principali: | , , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866908328188182528 |
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| author | Nabi, Jameel-Un Shehzadi, Ramoona Majid, Muhammad |
| author_facet | Nabi, Jameel-Un Shehzadi, Ramoona Majid, Muhammad |
| contents | Simulation studies indicate that weak interaction rates on nickel isotopes play a crucial role in determining the electron-to-baryon ratio within the stellar interior during the late stages of core evolution. (Anti)neutrinos produced through weak decay processes escape from stellar regions with densities below 10^11 g/cm^3, carrying away energy and thereby reducing the core entropy. In this work, we present a microscopic calculation of neutrino and antineutrino cooling rates resulting from weak interactions on nickel isotopes in the mass range 56 <= A <= 71. The calculations are performed using the deformed proton-neutron Quasiparticle Random Phase Approximation (pn-QRPA) model. Recent investigations into the Gamow-Teller (GT) strength distributions of nickel isotopes demonstrate that the deformed pn-QRPA model successfully reproduces experimental charge-changing transition data. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_14197 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Neutrino cooling rates due to nickel isotopes for presupernova evolution of massive stars Nabi, Jameel-Un Shehzadi, Ramoona Majid, Muhammad Nuclear Theory Simulation studies indicate that weak interaction rates on nickel isotopes play a crucial role in determining the electron-to-baryon ratio within the stellar interior during the late stages of core evolution. (Anti)neutrinos produced through weak decay processes escape from stellar regions with densities below 10^11 g/cm^3, carrying away energy and thereby reducing the core entropy. In this work, we present a microscopic calculation of neutrino and antineutrino cooling rates resulting from weak interactions on nickel isotopes in the mass range 56 <= A <= 71. The calculations are performed using the deformed proton-neutron Quasiparticle Random Phase Approximation (pn-QRPA) model. Recent investigations into the Gamow-Teller (GT) strength distributions of nickel isotopes demonstrate that the deformed pn-QRPA model successfully reproduces experimental charge-changing transition data. |
| title | Neutrino cooling rates due to nickel isotopes for presupernova evolution of massive stars |
| topic | Nuclear Theory |
| url | https://arxiv.org/abs/2504.14197 |