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\begin{document}

\title{Dynamical Heating in the Martian Thermosphere~}



\author[1]{Marcin Pilinski}%
\author[2]{K J Roeten}%
\author[2]{S W Bougher}%
\author[3]{M Benna}%
\affil[1]{Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, Colorado, USA}%
\affil[2]{Department of Climate and Space Sciences and Engineering, University of Michigan}%
\affil[3]{CRESST II, University of Maryland, Baltimore County}%


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  \date{May 26, 2024}


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\begin{abstract}
Dynamical heating and cooling are prominent features of planetary
atmospheres resulting in thermospheric structures on Venus, Earth and
Mars. The purpose of this study is to determine the location and
amplitude of localized heating regions in the Martian thermosphere,
confirm that they occur in regions of wind convergence, and to compare
the observed dynamical heating with that predicted by a global
thermospheric model. This investigation uses several years of data from
the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) mission
including observations made by the Neutral Gas and Ion Mass Spectrometer
(NGIMS) as well as the Extreme Ultraviolet Monitor (EUVM). Specifically,
the analysis focuses on several years of horizontal wind, temperature,
and composition data. EUVM measurements provide a solar forcing context
for the neutral thermosphere datasets and aid in the statistical
analysis. Statistical results are compared with two versions of the Mars
Global Ionosphere Thermosphere (M-GITM) global circulation model; one
that that includes gravity wave parametrization and a version without
gravity wave effects. Data analysis indicates that heating features
exists around 2-3 and 17-18 local solar time. These locations coincide
with regions of converging winds and are in better agreement with M GITM
when gravity wave parametrization is included in the model. A migrating
oscillation in the observed wind field also results in convergence and a
density enhancement near 15 local time. While a similar oscillation is
reproduced by the model, the amplitude is much lower than observed and
may be a result of modeled zonal winds that are too low.~%
\end{abstract}%



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