1. Cross Sections of the $^{83}$Rb(p,$γ)^{84}$Sr and $^{84}$Kr(p,$γ)^{85}$Rb Reactions at Energies Characteristic of the Astrophysical $γ$ Process
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Williams, M., Davids, B., Lotay, G., Nishimura, N., Rauscher, T., Gillespie, S. A., Alcorta, M., Amthor, A. M., Ball, G. C., Bhattacharjee, S. S., Bildstein, V., Catford, W. N., Doherty, D. T., Esker, N. E., Garnsworthy, A. B., Hackman, G., Hudson, K., Lennarz, A., Natzke, C., Olaizola, B., Psaltis, A., Svensson, C. E., Williams, J., Walter, D., and Yates, D.
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FOS: Physical sciences ,Nuclear Experiment (nucl-ex) ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
We have measured the cross section of the $^{83}$Rb(p,$γ)^{84}$Sr radiative capture reaction in inverse kinematics using a radioactive beam of $^{83}$Rb at incident energies of 2.4 and $2.7 A$ MeV. Prior to the radioactive beam measurement, the $^{84}$Kr(p,$γ)^{85}$Rb radiative capture reaction was measured in inverse kinematics using a stable beam of $^{84}$Kr at an incident energy of $2.7 A$ MeV. The effective relative kinetic energies of these measurements lie within the relevant energy window for the $γ$ process in supernovae. The central values of the measured partial cross sections of both reactions were found to be $0.17-0.42$ times the predictions of statistical model calculations. Assuming the predicted cross section at other energies is reduced by the same factor leads to a slightly higher calculated abundance of the $p$ nucleus $^{84}$Sr, caused by the reduced rate of the $^{84}$Sr($γ$,p)$^{83}$Rb reaction derived from the present measurement., 11 pages, 11 figures. arXiv admin note: text overlap with arXiv:2109.06775
- Published
- 2023
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