Energy rates due to Fe isotopes during presupernova evolution of massive stars
This work presents the microscopic calculation of energy rates (γ-ray heating and (anti)neutrino cooling rates) due to weak decay of selected Fe Isotopes. The isotopes have astrophysical significance during the presupernova evolution of massive stars. The energy rates are calculated using the pn-QRP...
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Veröffentlicht in: | New astronomy 2024-01, Vol.105, p.102114, Article 102114 |
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Sprache: | eng |
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Zusammenfassung: | This work presents the microscopic calculation of energy rates (γ-ray heating and (anti)neutrino cooling rates) due to weak decay of selected Fe Isotopes. The isotopes have astrophysical significance during the presupernova evolution of massive stars. The energy rates are calculated using the pn-QRPA model and compared with the independent particle model (IPM), large scale shell model (LSSM) and recent shell model calculation (GXPF1J). The reported (anti)neutrino cooling rates are smaller by up to two orders of magnitude at low core temperature values than the IPM rates. The two calculations compare well at T = 30 GK. The comparison of cooling rates with the LSSM is interesting. The pn-QRPA cooling rates due to even-even Fe isotopes are smaller (up to 2 orders of magnitude). For the odd-A isotopes, the reported rates are bigger up to an order of magnitude. The pn-QRPA computed cooling rates are, up to 2 orders of magnitude, bigger when compared with the GXPF1J calculation. The γ-ray heating rates due to electron capture rates rise with the temperature and density values of the stellar core. On the other hand, the γ-ray heating due to β-decay increases with the core temperature values but decreases by orders of magnitude when the stellar core stiffens. The pn-QRPA computed γ heating rates are bigger (up to 3 orders of magnitude) at high temperatures and densities (for the case of 55,56Fe) when compared with the recent shell model results. Owing to the importance of energy rates, this study may contribute to a realistic simulation of presupernova evolution of massive stars.
•pn-QRPA model is used to compute energy rates of Fe isotopes.•The energy rates are calculated without invoking Brink’s hypothesis.•The calculations are compared with the former results of IPM and LSSM.•The pn-QRPA computed energy rates are smaller than IPM rates at low core temperatures.•The reported rates are smaller (bigger) than LSSM results for even-even (odd-A) cases. |
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ISSN: | 1384-1076 1384-1092 |
DOI: | 10.1016/j.newast.2023.102114 |