Toward Understanding Polar Heat Transport Enhancement in Subglacial Oceans on Icy Moons
The interior oceans of several icy moons are considered as affected by rotation. Observations suggest a larger heat transport around the poles than at the equator. Rotating Rayleigh‐Bénard convection (RRBC) in planar configuration can show an enhanced heat transport compared to the non‐rotating case...
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| Vydáno v: | Geophysical research letters Ročník 51; číslo 3 |
|---|---|
| Hlavní autoři: | , , , |
| Médium: | Journal Article |
| Jazyk: | angličtina |
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Washington
John Wiley & Sons, Inc
16.02.2024
Wiley |
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| ISSN: | 0094-8276, 1944-8007 |
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| Abstract | The interior oceans of several icy moons are considered as affected by rotation. Observations suggest a larger heat transport around the poles than at the equator. Rotating Rayleigh‐Bénard convection (RRBC) in planar configuration can show an enhanced heat transport compared to the non‐rotating case within this “rotation‐affected” regime. We investigate the potential for such a (polar) heat transport enhancement in these subglacial oceans by direct numerical simulations of RRBC in spherical geometry for Ra = 106 and 0.7 ≤ Pr ≤ 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.
Plain Language Summary
The icy moons of Jupiter and Saturn like for example, Europa, Titan, or Enceladus are believed to have a water ocean beneath their ice crust. Several of them show phenomena in their polar regions like active geysers or a thinner crust than at the equator, all of which might be related to a larger heat transport around the poles from the underlying ocean. We simulate the flow dynamics and currents in these subglacial ocean by high‐fidelity simulations, though still at less extreme parameters than in reality, to study the heat transport and provide a possible explanation of such a “polar heat transport enhancement.” We find that the heat transport around the poles can be up to 50% larger than around the equator, and that the believed properties of the icy moons and their oceans would allow polar heat transport enhancement. Therefore, our results may help to improve the understanding of ocean currents and latitudinal variations in the oceanic heat transport and crustal thickness on icy moons.
Key Points
The polar heat transport in spherical rotating Rayleigh‐Bénard convection experiences an enhancement by rotation
The influence of rotation differs at low latitudes: the heat flux is reduced and compensates the polar enhancement on the global average
In combination, this strengthens the latitudinal variation between polar and equatorial heat flux for Prandtl numbers larger than unity |
|---|---|
| AbstractList | The interior oceans of several icy moons are considered as affected by rotation. Observations suggest a larger heat transport around the poles than at the equator. Rotating Rayleigh‐Bénard convection (RRBC) in planar configuration can show an enhanced heat transport compared to the non‐rotating case within this “rotation‐affected” regime. We investigate the potential for such a (polar) heat transport enhancement in these subglacial oceans by direct numerical simulations of RRBC in spherical geometry for
Ra
= 10
6
and 0.7 ≤
Pr
≤ 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.
The icy moons of Jupiter and Saturn like for example, Europa, Titan, or Enceladus are believed to have a water ocean beneath their ice crust. Several of them show phenomena in their polar regions like active geysers or a thinner crust than at the equator, all of which might be related to a larger heat transport around the poles from the underlying ocean. We simulate the flow dynamics and currents in these subglacial ocean by high‐fidelity simulations, though still at less extreme parameters than in reality, to study the heat transport and provide a possible explanation of such a “polar heat transport enhancement.” We find that the heat transport around the poles can be up to 50% larger than around the equator, and that the believed properties of the icy moons and their oceans would allow polar heat transport enhancement. Therefore, our results may help to improve the understanding of ocean currents and latitudinal variations in the oceanic heat transport and crustal thickness on icy moons.
The polar heat transport in spherical rotating Rayleigh‐Bénard convection experiences an enhancement by rotation
The influence of rotation differs at low latitudes: the heat flux is reduced and compensates the polar enhancement on the global average
In combination, this strengthens the latitudinal variation between polar and equatorial heat flux for Prandtl numbers larger than unity Abstract The interior oceans of several icy moons are considered as affected by rotation. Observations suggest a larger heat transport around the poles than at the equator. Rotating Rayleigh‐Bénard convection (RRBC) in planar configuration can show an enhanced heat transport compared to the non‐rotating case within this “rotation‐affected” regime. We investigate the potential for such a (polar) heat transport enhancement in these subglacial oceans by direct numerical simulations of RRBC in spherical geometry for Ra = 106 and 0.7 ≤ Pr ≤ 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. The interior oceans of several icy moons are considered as affected by rotation. Observations suggest a larger heat transport around the poles than at the equator. Rotating Rayleigh‐Bénard convection (RRBC) in planar configuration can show an enhanced heat transport compared to the non‐rotating case within this “rotation‐affected” regime. We investigate the potential for such a (polar) heat transport enhancement in these subglacial oceans by direct numerical simulations of RRBC in spherical geometry for Ra = 106 and 0.7 ≤ Pr ≤ 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. Plain Language Summary The icy moons of Jupiter and Saturn like for example, Europa, Titan, or Enceladus are believed to have a water ocean beneath their ice crust. Several of them show phenomena in their polar regions like active geysers or a thinner crust than at the equator, all of which might be related to a larger heat transport around the poles from the underlying ocean. We simulate the flow dynamics and currents in these subglacial ocean by high‐fidelity simulations, though still at less extreme parameters than in reality, to study the heat transport and provide a possible explanation of such a “polar heat transport enhancement.” We find that the heat transport around the poles can be up to 50% larger than around the equator, and that the believed properties of the icy moons and their oceans would allow polar heat transport enhancement. Therefore, our results may help to improve the understanding of ocean currents and latitudinal variations in the oceanic heat transport and crustal thickness on icy moons. Key Points The polar heat transport in spherical rotating Rayleigh‐Bénard convection experiences an enhancement by rotation The influence of rotation differs at low latitudes: the heat flux is reduced and compensates the polar enhancement on the global average In combination, this strengthens the latitudinal variation between polar and equatorial heat flux for Prandtl numbers larger than unity The interior oceans of several icy moons are considered as affected by rotation. Observations suggest a larger heat transport around the poles than at the equator. Rotating Rayleigh‐Bénard convection (RRBC) in planar configuration can show an enhanced heat transport compared to the non‐rotating case within this “rotation‐affected” regime. We investigate the potential for such a (polar) heat transport enhancement in these subglacial oceans by direct numerical simulations of RRBC in spherical geometry for Ra = 106 and 0.7 ≤ Pr ≤ 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. |
| Author | Stevens, Richard J. A. M. Lohse, Detlef Verzicco, Roberto Hartmann, Robert |
| Author_xml | – sequence: 1 givenname: Robert orcidid: 0000-0002-4860-0449 surname: Hartmann fullname: Hartmann, Robert email: r.hartmann@utwente.nl organization: University of Twente – sequence: 2 givenname: Richard J. A. M. orcidid: 0000-0001-6976-5704 surname: Stevens fullname: Stevens, Richard J. A. M. organization: University of Twente – sequence: 3 givenname: Detlef orcidid: 0000-0003-4138-2255 surname: Lohse fullname: Lohse, Detlef organization: Max Planck Institute for Dynamics and Self‐Organisation – sequence: 4 givenname: Roberto orcidid: 0000-0002-2690-9998 surname: Verzicco fullname: Verzicco, Roberto email: verzicco@uniroma2.it organization: Gran Sasso Science Institute |
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| CitedBy_id | crossref_primary_10_1016_j_icarus_2024_116441 crossref_primary_10_1016_j_icarus_2025_116807 crossref_primary_10_1007_s12217_025_10198_0 crossref_primary_10_1016_j_cpc_2025_109579 crossref_primary_10_1038_s43247_025_02036_3 |
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| Snippet | The interior oceans of several icy moons are considered as affected by rotation. Observations suggest a larger heat transport around the poles than at the... Abstract The interior oceans of several icy moons are considered as affected by rotation. Observations suggest a larger heat transport around the poles than at... |
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| SubjectTerms | Convection Crustal thickness Direct numerical simulation direct numerical simulations Enceladus Equator Europa Flow simulation Geysers Gravity Heat heat transfer Heat transport Hot springs Icy satellites Jovian Jupiter Jupiter satellites Latitudinal variations Numerical simulations Ocean currents Oceanic crust Oceans Polar environments Polar regions rotating flows Rotation Saturn Saturn satellites Saturnian satellites thermal convection Titan Turbulence |
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| Title | Toward Understanding Polar Heat Transport Enhancement in Subglacial Oceans on Icy Moons |
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