The role of subsurface ocean dynamics and phase transitions in forming the topography of icy moons
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10489452" target="_blank" >RIV/00216208:11320/24:10489452 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=gjbwhZb-c3" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=gjbwhZb-c3</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1016/j.icarus.2024.115985" target="_blank" >10.1016/j.icarus.2024.115985</a>
Alternative languages
Result language
angličtina
Original language name
The role of subsurface ocean dynamics and phase transitions in forming the topography of icy moons
Original language description
The thermo-mechanical evolution of icy moons cannot be understood without taking into account the complex interaction between the solid ice crust and the liquid water ocean. This interaction is controlled by the heat flux from the ocean and the material properties of ice. In recent years, the mass and energy exchange between the crust and the ocean has been studied using two complementary approaches. While in the first approach, the heat flux from the ocean is governed by the internal dynamics of the ocean and is independent of the processes at the phase boundary, the other approach assumes that the heat flux from the ocean is controlled by variations in the melting temperature along the boundary and the role of the ocean in heat transfer is passive. Here we present a new method for modeling the heat transfer in the interior of icy moons. Our approach is based on solving the heat transfer equations simultaneously in the ice shell and the ocean, and is more general than the previous ones in that it consistently links the global ocean circulation with the melting temperature variations arising from the deformation of the ice -water phase boundary. The method is used to study the role of ocean circulation in the formation of surface and ice -water interface topographies. We show that the additional heat flux generated by variations in the melting temperature along the phase boundary counteracts the heat flux from the deep ocean but is not able to completely suppress it. The deep ocean heat flux is more reduced at high latitudes than near the equator, where the ocean circulation is dominated by strong zonal flows hampering the heat transfer in the meridional direction. Our simulations predict the shape and topography that are comparable in magnitude to those observed on Titan (similar to 500 m) and explain the absence of a degree -2 sectoral component in the spherical harmonic expansion of Titan's topography.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10500 - Earth and related environmental sciences
Result continuities
Project
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Continuities
S - Specificky vyzkum na vysokych skolach
Others
Publication year
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Icarus
ISSN
0019-1035
e-ISSN
1090-2643
Volume of the periodical
412
Issue of the periodical within the volume
February
Country of publishing house
US - UNITED STATES
Number of pages
16
Pages from-to
115985
UT code for WoS article
001182152900001
EID of the result in the Scopus database
2-s2.0-85184588973