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\begin{document}

\title{Towards understanding polar heat transport enhancement in sub-glacial
oceans on icy moons}



\author[1]{Robert Hartmann}%
\author[1]{Richard J. A. M. Stevens}%
\author[1]{Detlef Lohse}%
\author[2]{Roberto Verzicco}%
\affil[1]{University of Twente}%
\affil[2]{Universita' di Roma Tor Vergata}%


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  \date{June 11, 2024}


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\selectlanguage{english}
\begin{abstract}
The interior oceans of several icy moons are considered as ``moderately
rotating''. Observations suggest a larger heat transport around the
poles than at the equator. Rotating Rayleigh-B\selectlanguage{ngerman}énard convection (RRBC) in
planar configuration is known to show an enhanced heat transport
compared to the non-rotating case for such ``moderate'' rotation. We
investigate the potential for such a (polar) heat transport enhancement
in these sub-glacial oceans by direct numerical simulations of RRBC in
spherical geometry for Ra=10\textsuperscript{6} and 0.7\selectlanguage{english}[?]Pr\selectlanguage{english}[?]4.38. We find
an enhancement up to 28\% in the ``polar tangent cylinder'', which is
globally compensated by a reduced heat transport at low latitudes. As a
result, the polar heat transport can exceed the equatorial by up to
50\%. The enhancement is mostly insensitive to different radial gravity
profiles, but decreases for thinner shells. In general, polar heat
transport and its enhancement in spherical RRBC follow the same
principles as in planar RRBC.%
\end{abstract}\selectlanguage{ngerman}%



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