Investigating the Impact of the Strontium Neutron-Capture Reaction Rates on i-Process Nucleosynthesis

The origin of elements in the universe is a longstanding open question in nuclear astrophysics. It is well known that most of the heavy elements greater than iron are synthesized via the traditional neutron-capture processes such as the slow (s) and rapid (r) processes. Recently a third process has come into the picture and is known as the intermediate (i) process. The i-process is less well known as compared to the two traditional neutron-capture processes. Some possible astrophysical sites containing conditions consistent with the i-process include CEMP stars, low metallicity, low mass super AGB or post AGB stars. Studies of neutron-capture reaction rates and their impact on i-process nucleosynthesis have been investigated and sensitivity studies have been performed. Recent advances in radioactive beam facilities have enabled researchers to experimentally constrain reaction rates such as the 93Sr(n,g)94Sr, which is important for the i-process. Here we use Hauser Feshbach formalism to calculate the 93Sr(n,g)94Sr reaction rate and implement it in a one-zone i-process simulation to investigate its significance for the i-process.