Exploring Jupiter's Aurorae with the Chandra and XMM-Newton X-ray Observatories

Jupiter's polar X-ray aurora is dominated by a bright dynamic hot spot that is produced by precipitating 10 MeV ions [Gladstone et al. 2002; Elsner et al. 2005; Branduardi-Raymont et al. 2007]. These highly energetic emissions exhibit pulsations over timescales of 10s of minutes and change morphology, intensity and precipitating particle populations from observation to observation and pole to pole [e.g. Dunn et al. 2017]. Surrounding the soft X-ray emission there is an oval of hard X-ray bremsstrahlung from precipitating electrons. The acceleration process/es that allow Jupiter to produce these high-energy X-ray emissions remain poorly understood, but vary with solar wind conditions [Dunn et al. 2016; Kimura et al. 2016] and the soft X-ray emissions are expected to relate to processes on the boundary between Jupiter's magnetosphere and the solar wind.We present a decade of remote X-ray observations of Jupiter from 2007 to 2017 using the Earth-orbiting X-ray telescopes Chandra and XMM-Newton. We compare these high spatial and spectral resolution X-ray data with in-situ measurements of the solar wind and the Jovian magnetosphere conducted by NASA's New Horizons and Juno spacecraft. Analysing X-ray spectrograms and X-ray auroral videos we probe time-varying accelerations, precipitating particle populations and auroral morphologies and further connect these with their solar wind and in-situ drivers. Finally, we compare X-ray observations with UV observations to enrich multi-waveband connections and deepen our understanding of how Jupiter generates its highly energetic polar auroral precipitations.