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\begin{document}

\title{Investigating the Linkage Between Spiral Trough Morphology and Cloud
Coverage on the Martian North Polar Layered Deposits}



\author[1]{Katherine Anne Lutz}%
\author[1]{Robert L Hawley}%
\author[1]{Marisa Christina Palucis}%
\affil[1]{Dartmouth College}%


\vspace{-1em}



  
  \date{May 15, 2024}


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\begin{abstract}
The Martian North Polar Layered Deposits (NPLD) are composed of
alternating water-ice and dust-rich layers resulting from atmospheric
deposition and are key to understanding Mars' climate cycles. Within
these deposits are spiral troughs, whose migration affects deposition
signals. To understand the relationship between NPLD stratigraphy and
Martian climate, we must identify modern-day drivers of NPLD ice
migration. Prevailing theory posits migration driven by
upstream-migrating bed undulations bounded by hydraulic jumps, caused by
katabatic winds flowing over trough walls with asymmetric
cross-sectional relief. This is supported by trough-parallel clouds,
whose formation has been attributed to hydraulic jumps.

We present a cloud atlas across the Martian north pole using
\textasciitilde{}13,800 THEMIS images spanning \textasciitilde{}18 Earth
years. We find trough-parallel clouds in \textasciitilde{}400 images,
with regions nearer to the pole having higher cloud frequency. We
compare spiral trough geometry to our cloud atlas and find regions with
trough-parallel clouds often correlate with metrics associated with
modern-day sublimation-deposition cycles (i.e., relief and asymmetry),
but not always. In some regions, troughs with morphologies conducive to
cloud formation have no clouds. Overall, trough geometry varies greatly
across the deposits, both within and between troughs, suggesting
localized differences in deposition relative to migration, varying
katabatic wind intensities, differing past climatic states influencing
the troughs, varying trough initiation properties, or the possibility of
additional mechanisms for trough initiation and migration (e.g., in-situ
trough erosion). Understanding what controls trough shape variability
across the NPLD and how these controls change through time and space is
key when interpreting Martian paleoclimate. Abstract content goes here%
\end{abstract}%



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