Constraining neutron-capture cross section for the i-process for the^151-153Nd(n,γ)^152-154Nd reaction via the β Oslo method

Nucleosynthesis of heavy elements has been traditionally attributed to two neutron-

capture processes, namely the s and r processes. Recent astronomical observations

have revealed stars where the abundance distributions cannot be described by the

aforementioned processes and for this reason the astrophysical i process was in-

troduced (i for intermediate between s and r). While we know neutron densities

are between the s and r process, the stellar site where it can occur has not yet

been clearly identified and that is largely because of the nuclear uncertainties. The

i process flow involves isotopes only a few steps from stability, and in this region

the main nuclear physics uncertainty comes from neutron-capture reaction rates.

Specifically neutron capture reactions on Nd isotopes have been identified as impor-

tant for the production of Eu and Sm. With this goal in mind, an experiment was

run at the ATLAS facility using the low-energy beams delivered from CARIBU to

constrain neutron-capture reactions of importance for the i process. β-decays and

their corresponding γ-rays were identified using the SuN detector and the SuNTAN

moving tape system. The β-decay of ^152−154Pr into ^152−154Nd was measured and

the β-Oslo method was used to extract the nuclear level density and γ-ray strength

function of ^152−154Nd; preliminary results from this experiment will be presented

here. From these statistical properties, ^151−153Nd(n,γ)^152−154Nd reaction cross sec-

tions and reaction rates will be constrained and their significance to the i process

will be presented.