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\begin{document}

\title{A laboratory model for iron snow in planetary cores}



\author[1]{Ludovic Huguet}%
\author[2]{Michael Le Bars}%
\author[3]{Renaud Deguen}%
\affil[1]{ISTerre, Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, IRD, Université Gustave Eiffel, 38000 Grenoble, France}%
\affil[2]{CNRS, Aix Marseille Univ, Centrale Marseille, IRPHE}%
\affil[3]{Univ. Grenoble Alpes,  Univ. Savoie Mont Blanc, CNRS, IRD, Univ. Gustave Eiffel, ISTerre,}%


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  \date{June 17, 2024}


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\begin{abstract}
Solidification of the cores of small planets and moons is thought to
occur in the \selectlanguage{ngerman}â\textbackslash{}euro\selectlanguage{english}~iron snow\selectlanguage{ngerman}â\textbackslash{}euro\selectlanguage{english}
regime, in which iron crystals form near the core-mantle boundary and
fall until re-melting at higher depth. The resulting buoyancy flux may
sustain convection and dynamo action. This regime is poorly known,
having never been observed in the field or laboratory. Here we present
the first laboratory experiments designed to model iron snow. We find
that solidification happens in a cyclic pattern, with intense
solidification bursts separated by crystal-free periods. This is
explained by the necessity of reaching a finite amount of supercooling
to re-initiate crystallization once the crystals formed earlier have
migrated away. When transposed to planetary cores, our results suggest
that crystallization and the associated buoyancy flux would be strongly
heterogeneous in time and space, which eventually impacts the time
variability and geometry of the magnetic field.%
\end{abstract}\selectlanguage{ngerman}%



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