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\begin{document}

\title{Hot Electron Temperature Layer in the Martian Atmosphere}



\author[1]{Laila Andersson}%
\author[2]{Christopher Fowler}%
\author[1]{Bob Ergun}%
\author[3]{Roger Yelle}%
\author[4]{Thomas Edward Cravens}%
\author[1]{Ed Thiemann}%
\author[1]{W. K. Peterson}%
\author[5]{Andy Nagy}%
\author[5]{Stephen Bougher}%
\author[6]{Mehdi Benna}%
\author[2]{David Mitchell}%
\author[2]{James McFadden}%
\affil[1]{University of Colorado}%
\affil[2]{University of California, Berkeley}%
\affil[3]{University of Arizona}%
\affil[4]{University of Kansas}%
\affil[5]{University of Michigan}%
\affil[6]{UNIVERSITY OF MARYLAND BALTIMORE CO}%


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  \date{May 18, 2024}


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\begin{abstract}
The MAVEN mission has measured an electron temperature spike at
altitudes where the Martian atmosphere becomes optically thick and
changes occur in the atmospheric chemistry. The temperature spike is
consistent from orbit to orbit, but changes in location based on solar
zenith angle (SZA) and has only been observed for SZA \textless{}80o.
This letter presents the conditions under which it is observed and
discusses possible sources. The electron temperature spike seems to be
co-located with a temperature dip in the neutral atmosphere. The
observed temperature spike/dip might be indicative of an inversion layer
in the Martian atmosphere. The altitude location of the electron
temperature spike is in the lower dynamo region where the electrons
start to be unmagnetized. The observations are unlikely to be
significant for overall Martian plasma dynamics, but are a clear
indication that the large-scale Martian atmosphere is still not
completely understood.%
\end{abstract}%



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