https://doi.org/10.1051/epjconf/202327502006
Astrophysical S factor and reaction rate of 92,94Mo(p, γ) relevant to the p-process
1 Department of Physics, Faculty of Science, The M. S. University of Baroda, Vadodara - 390002, India.
2 Manipal Centre for Natural Sciences,Manipal Academy of Higher Education, Manipal-576014, India.
3 Istituto Nazionale di Fisica Nucleare, Laboratori del Sud, Catania-95123, Italy.
4 Department of Physics, Manipal Institute of Technology, Manipal-576014, India.
5 Department of Electrical Power Engineering, Brno University of Technology, Brno, Czech Republic.
* e-mail: hinguaakash@gmail.com
** e-mail: pareshkumar.p@manipal.edu
*** e-mail: sk.mukherjee-phy@msubaroda.ac.in
Published online: 3 February 2023
Abstract. Low energy proton capture cross sections on heavy isotopes are necessary for a better understanding of the astrophysical p-process. There are around 35 proton-rich stable isotopes between 74S e and 196Hg which are bypassed by the s- and r- processes. These are commonly referred as p-nuclei whose origin is still not completely understood. In the present study, proton capture reactions are studied on Mo isotopes at astrophysically relevant energies using nuclear modular code TALYS. Astrophysical S factor and reaction rates are also calculated inside a core-collapse supernova. The obtained results are compared with the literature data taken from EXFOR data library. In addition, the effect of different combinations of the nuclear input parameters entering the stellar reaction rate have been investigated.
© The Authors, published by EDP Sciences, 2023
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
