Theβ-decay properties of^(67-80)As nuclei have been investigated within the framework of the proton-neutron quasi-particle random phase approximation(pn-QRPA)model.The nuclear deformation obtained from the finite ran...Theβ-decay properties of^(67-80)As nuclei have been investigated within the framework of the proton-neutron quasi-particle random phase approximation(pn-QRPA)model.The nuclear deformation obtained from the finite range droplet model is used as an input parameter in the pn-QRPA model for the analysis ofβ-decay properties including Gamow-Teller strength distributions,log ft,β-decay half-lives and stellarβ^(±)decay rates.The predicted log ft values were fairly consistent with the observed data.The computedβ-decay half-lives matched the measured values by a factor of 10.The stellar rates were compared with the shell model outcomes.At high densities and temperatures,theβ^(+)and electron capture rates had a finite contribution.However,theβ^(-)and positron capture rates are only significant at high temperatures and low densities.The pn-QRPA rates outperformed the shell model rates by a factor of 22 or more.展开更多
Key nuclear inputs for the astrophysical r-process simulations are the weak interaction rates.Consequently,the accuracy of these inputs directly affects the reliability of nucleosynthesis modeling.The majority of the ...Key nuclear inputs for the astrophysical r-process simulations are the weak interaction rates.Consequently,the accuracy of these inputs directly affects the reliability of nucleosynthesis modeling.The majority of the stellar rates,used in simulation studies are calculated by invoking the Brink-Axel(BA)hypothesis.The BA hypothesis assumes that the strength functions of all parent excited states are the same as for the ground state,only shifted in energies.However,the BA hypothesis has to be tested against microscopically calculated state-by-state rates.In this project,we study the impact of the BA hypothesis on calculated stellarβ^(-)-decay and electron capture rates.Our investigation include both unique first forbidden(U1F)and allowed transitions for 106 neutron-rich trans-iron nuclei([27,77]≤[Z,A]≤[82,208]).The calculations were performed using the deformed proton-neutron quasiparticle random-phase approximation(pn-QRPA)model with a simple plus quadrupole separable and schematic interaction.Waiting-point and several key r-process nuclei lie within the considered mass region of the nuclear chart.We computed electron capture andβ^(-)-decay rates using two different prescriptions for strength functions.One was based on invoking the BA hypothesis and the other was the state-by-state calculation of strength functions,under stellar density and temperature conditions([10,1]≤[ρYe(g/cm^(3)),T(GK)]≤[10^(11),30]).Our results show that the BA hypothesis invoked U1Fβ^(-)rates are overestimated by 4–5 orders of magnitude as compared to microscopic rates.For capture rates,more than two orders of magnitude differences were noted when applying the BA hypothesis.It was concluded that the BA hypothesis is not a reliable approximation,especially forβ^(-)-decay forbidden transitions.展开更多
基金funded by Taif University,Saudi Arabia,Project No.(TU-DSPP-2024-33)。
文摘Theβ-decay properties of^(67-80)As nuclei have been investigated within the framework of the proton-neutron quasi-particle random phase approximation(pn-QRPA)model.The nuclear deformation obtained from the finite range droplet model is used as an input parameter in the pn-QRPA model for the analysis ofβ-decay properties including Gamow-Teller strength distributions,log ft,β-decay half-lives and stellarβ^(±)decay rates.The predicted log ft values were fairly consistent with the observed data.The computedβ-decay half-lives matched the measured values by a factor of 10.The stellar rates were compared with the shell model outcomes.At high densities and temperatures,theβ^(+)and electron capture rates had a finite contribution.However,theβ^(-)and positron capture rates are only significant at high temperatures and low densities.The pn-QRPA rates outperformed the shell model rates by a factor of 22 or more.
基金supported by the Higher Education Commission Pakistan through Project (0-15394/NRPU/R&D/HEC/2021)。
文摘Key nuclear inputs for the astrophysical r-process simulations are the weak interaction rates.Consequently,the accuracy of these inputs directly affects the reliability of nucleosynthesis modeling.The majority of the stellar rates,used in simulation studies are calculated by invoking the Brink-Axel(BA)hypothesis.The BA hypothesis assumes that the strength functions of all parent excited states are the same as for the ground state,only shifted in energies.However,the BA hypothesis has to be tested against microscopically calculated state-by-state rates.In this project,we study the impact of the BA hypothesis on calculated stellarβ^(-)-decay and electron capture rates.Our investigation include both unique first forbidden(U1F)and allowed transitions for 106 neutron-rich trans-iron nuclei([27,77]≤[Z,A]≤[82,208]).The calculations were performed using the deformed proton-neutron quasiparticle random-phase approximation(pn-QRPA)model with a simple plus quadrupole separable and schematic interaction.Waiting-point and several key r-process nuclei lie within the considered mass region of the nuclear chart.We computed electron capture andβ^(-)-decay rates using two different prescriptions for strength functions.One was based on invoking the BA hypothesis and the other was the state-by-state calculation of strength functions,under stellar density and temperature conditions([10,1]≤[ρYe(g/cm^(3)),T(GK)]≤[10^(11),30]).Our results show that the BA hypothesis invoked U1Fβ^(-)rates are overestimated by 4–5 orders of magnitude as compared to microscopic rates.For capture rates,more than two orders of magnitude differences were noted when applying the BA hypothesis.It was concluded that the BA hypothesis is not a reliable approximation,especially forβ^(-)-decay forbidden transitions.
