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Identifying the Variety of Jovian X‐Ray Auroral Structures: Tying the Morphology of X‐Ray Emissions to Associated Magnetospheric Dynamics
Journal article   Open access   Peer reviewed

Identifying the Variety of Jovian X‐Ray Auroral Structures: Tying the Morphology of X‐Ray Emissions to Associated Magnetospheric Dynamics

D. M. Weigt, C. M. Jackman, D. Moral Pombo, S. V. Badman, C. K. Louis, W. R. Dunn, S. C. McEntee, G. Branduardi-Raymont, D. Grodent, M. F. Vogt, …
Journal of geophysical research. Space physics, Vol.128(11), e2023JA031656
11/2023
DOI: 10.1029/2023JA031656
url
https://doi.org/10.1029/2023JA031656View
Published (Version of record) Open Access

Abstract

Abstract We define the spatial clustering of X‐rays within Jupiter's northern auroral regions by classifying their distributions into “X‐ray auroral structures.” Using data from Chandra during Juno's main mission observations (24 May 2016 to 8 September 2019), we define five X‐ray structures based on their ionospheric location and calculate the distribution of auroral photons. The morphology and ionospheric location of these structures allow us to explore the possibility of numerous X‐ray auroral magnetospheric drivers. We compare these distributions to Hubble Space Telescope (HST) and Juno (Waves and MAG) data, and a 1D solar wind propagation model to infer the state of Jupiter's magnetosphere. Our results suggest that the five sub‐classes of “X‐ray structures” fall under two broad morphologies: fully polar and low latitude emissions. Visibility modeling of each structure suggests the non‐uniformity of the photon distributions across the Chandra intervals are likely associated with the switching on/off of magnetospheric drivers as opposed to geometrical effects. The combination of ultraviolet (UV) and X‐ray morphological structures is a powerful tool to elucidate the behavior of both electrons and ions and their link to solar wind/magnetospheric conditions in the absence of an upstream solar monitor. Although much work is still needed to progress the use of X‐ray morphology as a diagnostic tool, we set the foundations for future studies to continue this vital research. Plain Language Summary The mechanism that allows precipitation of ions into Jupiter's atmosphere and generate pulsed X‐ray auroral emissions is still under debate today. Previous studies have linked this driver to possible activity in Jupiter's outer magnetosphere (the interface between the solar wind and Jupiter) and have observed the emissions to exhibit variable behavior. More recent studies have suggested a wide range of physical phenomena causing these emissions. Here we explore this idea in more detail by introducing five “X‐ray auroral structures” that map to different regions in the Jovian system. Using data from the Chandra X‐ray Observatory during Juno's main mission allows us to calculate the distribution of X‐rays from Jupiter's northern auroral region. We compare our X‐ray results with the ultraviolet emissions (“UV auroral families”) observed from simultaneous Hubble Space Telescope (HST) data and infer the conditions at Jupiter using models and Juno observations. These “X‐ray structures” provide us with many ways to observe variable behavior and provide a possible tool to monitor the solar wind conditions, when used in tandem with the HST “UV auroral families.” Key Points We present the morphology of new “X‐ray auroral structures,” observed on Jupiter via Chandra's high spatial resolution camera We show that non‐uniform auroral photon distributions are likely from “switching on/off” of auroral driver(s) opposed to planetary tilt We show that combination of X‐ray and ultraviolet (UV) “auroral families” may be a useful proxy to determine the magnetospheric conditions at Jupiter

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