Probing Ion Precipitation at Jupiter's Poles Through Dynamic X-ray Spectra

Jupiter's polar regions produce dynamic multi-waveband auroras. The most energetic of these photons are X-rays [e.g Gladstone et al. 2002; Cravens et al. 2003; Elsner et al. 2005; Branduardi-Raymont et al. 2008; Dunn et al. 2017], which are dominantly produced by the collision of precipitating MeV ions with the atmosphere. The XMM-Newton observatory provides high spectral and temporal resolution of these emissions so that the energies and species of the precipitating ions may be identified at any given time. By analysing XMM observations coincident with NASA's Juno spacecraft's polar encounters and Hubble Ultraviolet and IRTF Infrared observations, we connect a variety of auroral morphologies with the ion species that produce them and the energies required for those specific X-ray lines [e.g. Ozak et al. 2013; Houston et al. 2018]. Oxygen and sulphur ions with time-varying charge states (O⁷⁺ to O⁸⁺; S⁷⁺ to S¹⁶⁺) have been identified as producing X-rays in the polar regions [e.g. Branduardi-Raymont et al. 2007; Haggerty et al. 2017], but alongside these ions there are an array of spectral lines that do not appear to be oxygen or sulphur lines. We begin to utilise Bayesian and deep learning techniques to identify the ions responsible for these low-signal X-ray auroral lines. By doing this, we hope to constrain the source of the precipitations and the physical processes that produce Jupiter's most energetic auroral photons.