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\begin{document}

\title{Volumetric changes of mud on Mars: evidence from laboratory simulations}



\author[1]{Petr Brož}%
\author[1]{Ondřej Krýza}%
\author[2]{Vojtech Patocka}%
\author[3]{Věra Pěnkavová}%
\author[4]{Susan J Conway}%
\author[5]{Adriano Mazzini}%
\author[6]{Ernst Hauber}%
\author[7]{Matthew E. Sylvest}%
\author[7]{Manish R Patel}%
\affil[1]{Institute of Geophysics CAS, v.v.i.}%
\affil[2]{Charles University}%
\affil[3]{Institute of Chemical Process Fundamentals of the Czech Academy of Sciences, Prague, Czech Republic}%
\affil[4]{University of Nantes}%
\affil[5]{Centre for Earth Evolution and Dynamics}%
\affil[6]{DLR}%
\affil[7]{The Open University}%


\vspace{-1em}



  
  \date{May 27, 2024}


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\begin{abstract}
Subtle mounds have been discovered in the source areas of martian
kilometer-sized flows and on top of summit areas of domes. These
features have been suggested to be related to subsurface sediment
mobilization, opening questions regarding their formation mechanisms.
Previous studies hypothesized that they mark the position of feeder
vents through which mud was brought to the surface. Two theories have
been proposed: a) ascent of more viscous mud during the late stage of
eruption and b) expansion of mud within the conduit due to the
instability of water under martian conditions. Here we present
experiments performed inside a low-pressure chamber, designed to
investigate whether the volume of mud changes when exposed to a reduced
atmospheric pressure. Depending on the mud viscosity, we observe
volumetric increase of up to 30\% at the martian average pressure of
\textasciitilde{}6 mbar. This is because the low pressure causes
instability of the water within the mud, leading to the formation of
bubbles that increase the volume of the mixture. This mechanism bears
resemblance to the volumetric changes associated with the degassing of
terrestrial lavas or mud volcano eruptions caused by a rapid pressure
drop. We conclude that the mounds associated with putative martian
sedimentary volcanoes might indeed be explained by volumetric changes of
the mud. We also show that mud flows on Mars and elsewhere in the Solar
System could behave differently to those found on Earth, because mud
dynamics are affected by the formation of bubbles in response to the low
atmospheric pressure.%
\end{abstract}%



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\verb`965555_0_supp_11068756_rvx942.docx`  available at \url{https://authorea.com/users/628332/articles/648948-volumetric-changes-of-mud-on-mars-evidence-from-laboratory-simulations}\selectlanguage{english}
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