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\begin{document}

\title{Global crustal thickness revealed by surface waves orbiting Mars}



\author[1]{Doyeon Kim}%
\author[2]{Cecilia Duran}%
\author[2]{Domenico Giardini}%
\author[3]{Ana-Catalina Plesa}%
\author[4]{Simon C. Stähler}%
\author[5]{Christian Boehm}%
\author[6]{Vedran Lekic}%
\author[7]{Scott M. McLennan}%
\author[8]{Savas Ceylan}%
\author[9]{John Clinton}%
\author[10]{Paul McEwan Davis}%
\author[11]{Amir Khan}%
\author[12]{Brigitte Knapmeyer-Endrun}%
\author[13]{Mark Paul Panning}%
\author[14]{Mark A. Wieczorek}%
\author[15]{Philippe Lognonné}%
\affil[1]{Swiss Federal Institute of Technology in Zürich}%
\affil[2]{ETH Zürich}%
\affil[3]{German Aerospace Center}%
\affil[4]{Eidgenössische Technische Hochschule Zürich}%
\affil[5]{Department of Earth Sciences, Institute of Geophysics, ETH Zürich}%
\affil[6]{University of Maryland, College Park}%
\affil[7]{Stony Brook University}%
\affil[8]{ETH Zurich}%
\affil[9]{Swiss Seismological Service}%
\affil[10]{University of California Los Angeles}%
\affil[11]{Swiss Federal Institute of Technology}%
\affil[12]{Bensberg Observatory, University of Cologne}%
\affil[13]{Jet Propulsion Laboratory, California Institute of Technology}%
\affil[14]{Université Paris Cité}%
\affil[15]{Université Paris Cité, Institute de physique de globe de Paris, CNRS}%


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  \date{May 25, 2024}


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\begin{abstract}
We report observations of Rayleigh waves that orbit around Mars up to
three times following the S1222a marsquake. Averaging these signals, we
find the largest amplitude signals at 30 s and 85 s central period,
propagating with distinctly different group velocities of 2.9 km/s and
3.8 km/s, respectively. The group velocities constraining the average
crustal thickness beneath the great circle path rule out the majority of
previous crustal models of Mars that have a \textgreater{}200 kg/m3
density contrast across the dichotomy. We find that the thickness of the
martian crust is 42-56 km on average, and thus thicker than the crusts
of the Earth and Moon. Together with thermal evolution models, a thick
martian crust suggests that the crust must contain 50-70\% of the total
heat production to explain present-day local melt zones in the interior
of Mars.%
\end{abstract}%



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