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\begin{document}

\title{Identifying the variety of jovian X-ray auroral structures: tying the
morphology of X-ray emissions to associated magnetospheric dynamics}



\author[1]{Dale Michael Weigt}%
\author[2]{Caitriona M Jackman}%
\author[3]{Diego Moral Pombo}%
\author[4]{Sarah V Badman}%
\author[1]{Corentin Kenelm Louis}%
\author[5]{William Dunn}%
\author[2]{Seán Christopher McEntee}%
\author[5]{Graziella Branduardi-Raymont}%
\author[6]{Denis Grodent}%
\author[7]{Marissa F. Vogt}%
\author[8]{Chihiro Tao}%
\author[9]{Randy Gladstone}%
\author[10]{Ralph P. Kraft}%
\author[11]{William S Kurth}%
\author[12]{John E. P. Connerney}%
\affil[1]{Dublin Institute for Advanced Studies (DIAS)}%
\affil[2]{Dublin Institute for Advanced Studies}%
\affil[3]{University of Lancaster}%
\affil[4]{Lancaster University}%
\affil[5]{University College London}%
\affil[6]{Université de Liège}%
\affil[7]{Boston University}%
\affil[8]{National Institute of Information and Communications Technology (NICT)}%
\affil[9]{Southwest Research Institute}%
\affil[10]{Smithsonian Astrophysical Observatory (SI)}%
\affil[11]{University of Iowa}%
\affil[12]{NASA Goddard Space Flight Center}%


\vspace{-1em}



  
  \date{May 21, 2024}


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\begin{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 -- 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 modelling 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 behaviour of both electrons and ions and their link to
solar wind/magnetospheric conditions in the absence of an upstream solar
monitor.%
\end{abstract}%



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