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\begin{document}

\title{Hydrogenation of the Martian Core by Hydrated Mantle Minerals with
Implications for the Early Dynamo}



\author[1]{Joseph Ghilarducci O'Rourke}%
\author[1]{Sang-Heon Shim}%
\affil[1]{Arizona State University}%


\vspace{-1em}



  
  \date{May 25, 2024}


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\begin{abstract}
Mars lacks an internally generated magnetic field today. Crustal
remanent magnetism and meteorites indicate that a dynamo existed after
accretion but died roughly four billion years ago. Standard models rely
on core/mantle heat flow dropping below the adiabatic limit for thermal
convection in the core. However, rapid core cooling after the Noachian
is favored instead to produce long-lived mantle plumes and magmatism at
volcanic provinces such as Tharsis and Elysium. Hydrogenation of the
core could resolve this apparent contradiction by impeding the dynamo
while core/mantle heat flow is super-adiabatic. Here we present
parameterized models for the rate at which mantle convection delivers
hydrogen into the core. Our models suggest that most of the water that
the mantle initially contained was effectively lost to the core. We
predict that the mantle became increasingly iron-rich over time and a
stratified layer awaits detection in the uppermost core---analogous to
the E' layer atop Earth's core but likely thicker than alternative
sources of stratification in the Martian core such as iron snow.
Entraining buoyant, hydrogen-rich fluid downwards in the core subtracts
gravitational energy from the total dissipation budget for the dynamo.
The calculated fluxes of hydrogen are high enough to potentially reduce
the lifetime of the dynamo by several hundred million years or longer
relative to conventional model predictions. Future work should address
the complicated interactions between the stratified, hydrogen-rich layer
and convection in the underlying core.%
\end{abstract}%



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