Abstract. A direct measurement of the 19 Ne(p, γ) 20 Na reaction has been performed in inverse kinematics at the DRAGON recoil separator, at an energy ∼ 10 keV higher than previous measurements. The key resonance in the 19 Ne +p system relevant for ONe novae and Type-I X-ray burst temperatures have been successfully measured for the first time. Preliminary estimates of the resonance energy and strength are reported as E c.m. ≈ 458 keV and ωγ ≈ 18 meV. These results are consistent with previous direct measurements, but disagree with the most recent study of the 19 Ne(p, γ) 20 Na reaction rate. These preliminary results will be finalised after a forthcoming negative log-likelihood analysis.Classical novae and X-ray bursts are among the most common types of explosive stellar phenomena observed in our Galaxy. These cataclysmic binary systems are stellar environments with high temperatures and densities, thought to be active regions of ongoing nucleosynthesis which energetically impact the surrounding interstellar medium (ISM).Classical novae are binary systems where hydrogen-rich material is accreted from a main sequence or red giant branch star onto the surface of a companion white dwarf. As the accreted material mixes with the heavier elements already present on the surface of the white dwarf, a thermonuclear runaway is triggered, which leads to explosive mass ejections from the white dwarf's surface, with the process recurring over a time-scale of ∼ 10 4 -10 5 years [1]. The composition of the white dwarf star has a significant impact on the composition of the nova ejecta; novae with more massive oxygen-neon (ONe) white dwarfs are characterised by higher peak temperatures (∼ 0.4 GK) than less massive carbon-oxygen (CO) white dwarfs (∼ 0.2 GK), and are thus thought to synthesise elements up to the Si-Ca mass region [2]. Therefore, determining the nature of the underlying white dwarf is crucial to meaningfully compare theoretical calculations with astronomical data.