One day after the discovery of the 2018 classical nova (CN) eruption of V392 Persei, a gamma-ray signal was detected from the position of V392 Per by the Fermi Gamma-Ray Space Telescope’s Large Area Telescope, sparking a panchromatic campaign of photometric and spectroscopic observations. As one of sixteen novae to date with detected gamma-ray emission, V392 Per provided an opportunity to probe the mechanism of the emission. This emission is thought to be due to particle acceleration by shocks between two or more different nova ejecta components, produced in multiple ejection episodes early in the eruption.

V392 Per, a known dwarf nova (DN), is the only DN whose subsequent CN eruption was detected in gamma-rays. It is one of only two DNe to later exhibit a CN eruption, and one of only nine cataclysmic variables to show clear evidence of both DN outbursts and a CN eruption. Archival observations available from the American Association of Variable Star Observers database, spanning over a decade, provide further information about the accretion history of the system.

A crucial component of the observing strategy was the use of the Neil Gehrels Swift Observatory, utilising its UV photometry and X-ray spectroscopy. I will present these observations, along with coordinated optical photometry and spectroscopy from ground based telescopes – spearheaded by the Liverpool Telescope – and discuss their significance.