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\begin{document}

\title{Marsquake locations and 1-D seismic models for Mars from InSight data}



\author[1,1]{Mélanie Drilleau}%
\author[2,2]{Henri Samuel}%
\author[3,3]{Raphaël F. Garcia}%
\author[4,4]{Attilio Rivoldini}%
\author[5,5]{Clément Perrin}%
\author[6,6]{Chloé Michaut}%
\author[7,7]{Mark Wieczorek}%
\author[6,6]{Benoît Tauzin}%
\author[8,8]{James A. D. Connolly}%
\author[9,9]{Pauline Meyer}%
\author[2,2]{Philippe Lognonné}%
\author[10,10]{William B. Banerdt}%
\affil[1]{Institut Supérieur de l’Aéronautique et de l’Espace ISAE-SUPAERO}%
\affil[2]{Institut de Physique du Globe de Paris, CNRS, Université de Paris, 1 rue Jussieu, 75005 Paris - France}%
\affil[3]{Institut Supérieur de l’Aéronautique et de l’Espace ISAE-SUPAERO, 10 Avenue Edouard Belin, 31400 Toulouse, France}%
\affil[4]{Royal Observatory of Belgium, Brussels, Belgium}%
\affil[5]{Nantes Université, Université d’Angers, Le Mans Université, CNRS UMR 6112, Laboratoire de Planétologie et Géosciences, UAR 3281, Observatoire des Sciences de l’Univers de Nantes Atlantique, F-44000 Nantes, France}%
\affil[6]{Université de Lyon, Ecole Normale Supérieure de Lyon, Université Claude Bernard Lyon 1, CNRS, Laboratoire de Géologie de Lyon : Terre, Planètes, Environnement, 69622 Villeurbanne, France}%
\affil[7]{Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France.}%
\affil[8]{Institute of Geophysics, ETH Zurich, Sonneggstrasse 5, Zurich, Switzerland}%
\affil[9]{Ecole et Observatoire des Sciences de la Terre, Université de Strasbourg, 5 rue René Descartes, 67084 Strasbourg, France}%
\affil[10]{Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA}%


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  \date{June 15, 2024}


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\begin{abstract}
We present inversions for the structure of Mars using the first Martian
seismic record collected by the InSight lander. We identified and used
arrival times of direct, multiples, and depth phases of body waves, for
seventeen marsquakes to constrain the quake locations and the
one-dimensional average interior structure of Mars. We found the
marsquake hypocenters to be shallower than 40 km depth, most of them
being located in the Cerberus Fossae graben system, which could be a
source of marsquakes. Our results show a significant velocity jump
between the upper and the lower part of the crust, interpreted as the
transition between intrusive and extrusive rocks. The lower crust makes
up a significant fraction of the crust, with seismic velocities
compatible with those of mafic to ultramafic rocks. Additional
constraints on the crustal thickness from previous seismic analyses,
combined with modeling relying on gravity and topography measurements,
yield constraints on the present-day thermochemical state of Mars and on
its long-term history. Our most constrained inversion results indicate a
present-day surface heat flux of 22\selectlanguage{ngerman}±1 mW/m2, a relatively hot mantle
(potential temperature: 1740±90 K) and a thick lithosphere (540±120 km),
associated with a lithospheric thermal gradient of 1.9±0.3 K/km. These
results are compatible with recent seismic studies using a reduced data
set and different inversions approaches, confirming that Mars' mantle
was initially relatively cold (1780±50 K) compared to its present-day
state, and that its crust contains 10-12 times more heat-producing
elements than the primitive mantle.%
\end{abstract}\selectlanguage{ngerman}%



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