Measuring the astrophysical ²⁰Ne(p, γ)²¹Na rate at DRAGON

Understanding the abundance levels of isotopes produced in oxygen-neon (ONe) novae within our galaxy requires accurate measurements of nuclear reaction rates within their associated reaction network. During these cataclysmic events, the produced radioisotope ²²Na is ejected into the interstellar medium and β-decays predominately to the first excited state in ²²Ne leading to a characteristic 1.275 MeV γ-ray. To date, there has been no astronomical observation of this characteristic γ-ray that can be a potential probe into the physics occuring within novae. The production of ²²Na in classical novae is limited by the ²⁰Ne(p, γ)²¹Na nuclear reaction that sets the focus of this experiment. Using the DRAGON recoil separator, new measurements of the ²⁰Ne(p, γ)²¹Na reaction are performed at lower energies closer to astrophysically relevant energy ranges. The aim is to reduce experimental uncertainties in the ²⁰Ne(p, γ)²¹Na reaction rate in order to more accurately predict the production yield of ²²Na in ONe novae and to measure the direct capture to the ground state in order to constrain the astrophysical S-factor. Experimental methods and preliminary results to be discussed.