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\title{EMM EMUS Observations of Hot Oxygen Corona at Mars: Radial Distribution
and Temporal Variability}



\author[1]{Krishnaprasad Chirakkil}%
\author[2]{Justin Deighan}%
\author[2]{Michael Scott Chaffin}%
\author[2]{Sonal Jain}%
\author[3]{Robert James Lillis}%
\author[4]{Susarla Raghuram}%
\author[1]{Gregory Holsclaw}%
\author[1]{David Andrew Brain}%
\author[5]{Edward Michael Benjamin Thiemann}%
\author[6]{Phillip C Chamberlin}%
\author[3]{Matthew O. Fillingim}%
\author[7]{Joseph Scott Evans}%
\author[8]{Scott L England}%
\author[9]{Hessa Almatroushi}%
\author[10]{Hoor Almazmi}%
\author[5]{Francis G. Eparvier}%
\author[11]{Marko Gacesa}%
\author[12]{Nayla El-Kork}%
\author[13]{Shannon M. Curry}%
\affil[1]{University of Colorado Boulder}%
\affil[2]{LASP}%
\affil[3]{University of California, Berkeley}%
\affil[4]{LASP, University of Colorado at Boulder}%
\affil[5]{Laboratory for Atmospheric and Space Physics}%
\affil[6]{University of Colorado, Laboratory for Atmospheric and Space Physics}%
\affil[7]{Computational Physics, Incorporated}%
\affil[8]{Virginia Polytechnic Institute and State University}%
\affil[9]{Unknown}%
\affil[10]{UAE Space Agency}%
\affil[11]{Bay Area Environmental Research Institute}%
\affil[12]{Khalifa University}%
\affil[13]{UC Berkeley}%


\vspace{-1em}



  
  \date{May 09, 2026}


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\begin{abstract}
We present the first observations of the dayside coronal oxygen emission
in far ultraviolet (FUV) measured by the Emirates Mars Ultraviolet
Spectrometer (EMUS) onboard the Emirates Mars Mission (EMM). The high
sensitivity of EMUS is providing an opportunity to observe the tenuous
oxygen corona in FUV, which is otherwise difficult to observe. Oxygen
resonance fluorescence emission at 130.4 nm provides a measurement of
the upper atmospheric and exospheric oxygen. More than 500 oxygen corona
profiles are constructed using the long-exposure time cross-exospheric
mode (OS4) of EMUS observations. These profiles range from
\textasciitilde{}200 km altitude up to several Mars radii
(\textgreater{}6 R\textsubscript{M}) across all seasons and for two Mars
years. Our analysis shows that OI 130.4 nm is highly correlated with
solar irradiance (solar photoionizing and 130.4 nm illuminating
irradiances) as well as changes in the Sun-Mars distance. The prominent
short term periodicity in oxygen corona brightness is consistent with
the solar rotation period (quasi-27-days). A comparison between the
perihelion seasons of Mars Year (MY) 36 and MY 37 shows interannual
variability with enhanced emission intensities during MY 37, due to the
rise of Solar Cycle 25. These observations show a highly variable oxygen
corona, which has significant implications on constraining the
photochemical escape of atomic oxygen from Mars.%
\end{abstract}%



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