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\begin{document}

\title{Statistical Analysis of Discrete Aurora on Mars: Variability with
Magnetic Topology, Local Time and Season}



\author[1]{Krishnaprasad Chirakkil}%
\author[2]{Robert James Lillis}%
\author[3]{Justin Deighan}%
\author[3]{Michael Scott Chaffin}%
\author[3]{Sonal Jain}%
\author[1]{David Andrew Brain}%
\author[2]{Matthew O. Fillingim}%
\author[4]{Raghuram Susarla}%
\author[1]{Gregory Holsclaw}%
\author[1]{Xiaohua Fang}%
\author[1]{Nicholas M. Schneider}%
\author[5]{Hoor Almazmi}%
\author[6]{Hessa Almatroushi}%
\author[7]{Marko Gacesa}%
\author[7]{Nayla El-Kork}%
\affil[1]{University of Colorado Boulder}%
\affil[2]{University of California, Berkeley}%
\affil[3]{LASP}%
\affil[4]{Laboratory for Atmospheric and Space Physics, University of  Colorado}%
\affil[5]{UAE Space Agency}%
\affil[6]{Unknown}%
\affil[7]{Khalifa University}%


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  \date{May 25, 2024}


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\begin{abstract}
We present a comprehensive study of the nightside discrete electron
aurora phenomenon on Mars, utilizing observations from EMUS onboard EMM.
The oxygen emission at 130.4 nm is by far the brightest FUV auroral
emission line observed at Mars. We identify auroral pixels in OI 130.4
nm disk observations, with higher sensitivity than previously possible.
Our statistical analysis reveals regional, SZA, local time, and seasonal
dependencies of auroral occurrence. Higher occurrence of aurora is
observed in regions of open magnetic topology and vertical crustal
magnetic fields. Aurora occurs more frequently closer to the terminator
and is more likely on the dusk versus dawn sides of the night
hemisphere. A pronounced auroral feature appears close to midnight local
times in the southern hemisphere, consistent with the ``spot'' of
energetic electron fluxes previously identified in the MGS data. The
auroral spot is more frequent after midnight than before. Additionally,
some regions on Mars are ``aurora voids'' where essentially no aurora
occurs. The non-crustal field aurora exhibits a seasonal dependence,
with major enhancements around Ls 235\selectlanguage{ngerman}° (near perihelion) and Ls 30°.
This is in line with the seasonal variability in ionospheric TEC
observed by Mars Express, which is in turn related to the variability of
solar irradiance and thermospheric density. Aurora occurrence also shows
an increase with the rise of Solar Cycle 25. These observations not only
shed light on where and when Martian aurora occurs, but also add to our
understanding of Mars' magnetic environment and its interaction with the
heliospheric environment.%
\end{abstract}\selectlanguage{ngerman}%



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