Jupiter's X‐ray Aurorae. A High Signal Spectral Analysis of the 0.24–1.40 keV Energy Range

Abstract Jupiter's X‐ray auroras are predominantly produced by precipitating energetic heavy ions. Recent results suggest a connection between the pulsation rate of these ion aurorae and the pulsation rate of magnetospheric waves. Using remote X‐ray observations and results from in situ measurements from the Juno Jupiter Energetic particle Detector Instrument (JEDI), this study investigates if ion species from the JEDI results are precipitating into the auroral regions of Jupiter, contributing to the X‐ray aurorae. This work investigates high signal X‐ray spectra from the northern and southern auroral regions of Jupiter using the XMM‐Newton X‐ray telescope. A model is developed, incorporating the ion species oxygen, neon, magnesium, silicon, and sulfur, consistent with the JEDI ion species, along with a fixed Astrophysical Plasma Emission Code model, a constrained power law model, and a velocity shift model. The model agrees with the co‐added spectra from the northern and southern aurora. The fitted velocity shift in the northern auroral region of Jupiter of −5,000 km/s agrees well with previous results obtained from the XMM‐Newton Reflection Grating Spectrometer that identified emission line broadening.