Speaker
Description
In this work, we re-assess the $^{65\!\!}$As(p,$\gamma$)$^{66\!}$Se reaction rates based on a set of proton thresholds of $^{66\!}$Se, $S_\mathrm{p}$($^{66\!}$Se), estimated from the experimental mirror nuclear masses, theoretical mirror displacement energies, and full $p\!f$-model space shell-model calculation. The mirror displacement energies with much reduced uncertainty of the self-consistent relativistic Hartree-Bogoliubov calculations, and thus reducing the proton-threshold uncertainty up to 161~keV compared to the AME2020 evaluation. Using the simulation instantiated by the one-dimensional multi-zone hydrodynamic code, \textsc{Kepler}, which follows the trend of the observed GS~1826$-$24 clocked bursts, the present forward and reverse $^{65\!\!}$As(p,$\gamma$)$^{66\!}$Se reaction rates based on a selected $S_\mathrm{p}$($^{66\!}$Se) $=2.469\mathord\pm0.054$~MeV, and the latest $^{22}$Mg($\alpha$,p)$^{25}\!$Al, $^{56}$Ni(p,$\gamma$)$^{57}$Cu, $^{57}$Cu(p,$\gamma$)$^{58}$Zn, $^{55}$Ni(p,$\gamma$)$^{56}$Cu, and $^{64}$Ge(p,$\gamma$)$^{65\!\!}$As reaction rates, we study the waiting point status of and two-proton sequential capture on $^{64}$Ge, weak-cycle feature of GeAs at region heavier than $^{64}$Ge, and impact of other possible $S_\mathrm{p}$($^{66\!}$Se), which could be a reference for future nuclear mass measurements.
| Please select a main topic related to your abstract | Theoretical Nuclear Physics for Astrophysics |
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