Love numbers for Io with a magma ocean
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10508247" target="_blank" >RIV/00216208:11320/25:10508247 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=5xqFkIvwM0" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=5xqFkIvwM0</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1016/j.icarus.2025.116567" target="_blank" >10.1016/j.icarus.2025.116567</a>
Alternative languages
Result language
angličtina
Original language name
Love numbers for Io with a magma ocean
Original language description
The volcanic activity of Jupiter's moon Io is driven by the heat generated by tidal deformation induced by its orbital resonance with Europa and Ganymede. The question of whether tidal dissipation primarily occurs in a partially molten solid layer ("magmatic sponge") or in a hypothetical liquid magma ocean has long been a subject of debate. The data collected by the Juno spacecraft during two recent flybys of Io has allowed, for the first time, to quantify Io's tidal deformation. The analysis of the data by Park et al. (2024) reveals that the Love number k(2) is about 0.125 and the tidal dissipation parameter Q is about 11.4. These values are compatible with a solid mantle but they do not exclude the possibility that a global magma ocean exists in the deep (>320 km) interior. Using a model based on the solution of the Navier-Stokes equation, we investigate the dependence of the Love number on the position of the ocean and examine how much it is affected by the Coriolis force, an effect that was not included in the study of Park et al. (2024). Varying the viscosity of the magma, the depth and the thickness of the ocean in the range of 10(2)-10(7) Pas, 50-400 km and 0.1-20 km, respectively, and considering only the models with a dissipation power of about 100 TW, we show that a magma ocean located at a depth of less than or similar to 200 km predicts either too large k2 or too long time lag, implying that the existence of a shallow magma ocean in Io is unlikely. A thin (<10 km) magma ocean located at a depth of less than or similar to 250 km is compatible with the observation and could, in principle, be detected by accurate measurement of degree 2 zonal and sectorial Love numbers. Our results are in general agreement with those of Park et al. (2024), indicating that Io's enormous volcanic activity is unlikely to be driven by a global fluid magma ocean located at a shallow depth. This conclusion is conditioned by the reliability of the method used to interpret the Juno data. As the tidal response of Io with a magma ocean is affected by the Coriolis force, the Love number depends on the harmonic order, which can complicate the analysis of the information collected during the flybys. The effect of fluid tides was not considered in the data processing, and therefore, the conclusions of Park et al. (2024) cannot be definitely confirmed.
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
2025
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
436
Issue of the periodical within the volume
March
Country of publishing house
US - UNITED STATES
Number of pages
7
Pages from-to
116567
UT code for WoS article
001465551500001
EID of the result in the Scopus database
2-s2.0-105001683125