Abstract
Cross sections of the 107Ag(α, γ)111In and 107Ag(α,n)110In reactions have been measured with the activation method at effective center-of-mass energies between 7.79 MeV and 12.00 MeV close to the astrophysical energy range. The irradiation and counting of the 107Ag targets was carried out at ATOMKI using the cyclotron accelerator and the low background counting facility, respectively. Cross section results are presented and compared with the predictions of Hauser-Feshbach statistical model calculations using the NON-SMOKER and TALYS-1.4 codes. In general, above 10 MeV, the model calculation are able to reproduce reasonably well the experimental data, but below 10 MeV, depending on some input parameters strong deviations are also found.
Highlights
The so-called astrophysical p process, which is responsible for production of about 35 rare nuclei along the proton-rich side of the stability line, is one of the least known among those processes which describe the synthesis of elements heavier than iron [1, 2, 3] The p process nucleosynthesis is modeled by using an extended nuclear reaction network, for which reaction rate information of thousands of neutron, proton and α-induced reactions as well as their inverse reactions is needed
In order to extend the experimental database for the astrophysical p process and to test the reliability of statistical model predictions in this mass range, cross sections of 107Ag(α,γ)111In and 107Ag(α,n)110In reactions have been measured with the activation method at effective centerof-mass energies between 7.79 MeV and 12.00 MeV, close to the astrophysical energy range
The 107Ag(α,γ)111In and 107Ag(α,n)110In reaction cross sections have been measured at laboratory energies between 8.16 MeV and 12.50 MeV, which include a part of the astrophysically relevant energy range
Summary
The so-called astrophysical p process, which is responsible for production of about 35 rare nuclei along the proton-rich side of the stability line, is one of the least known among those processes which describe the synthesis of elements heavier than iron [1, 2, 3] The p process nucleosynthesis is modeled by using an extended nuclear reaction network, for which reaction rate information of thousands of neutron, proton and α-induced reactions as well as their inverse reactions is needed. Astrophysical reaction rates are mostly derived from theoretical cross sections owing to the lack of experimental data. Experiments performed so far have shown that there are considerable differences between predictions and experimental cross sections [4, 5, 6].
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
