Tidal Heating in a Subsurface Magma Ocean on Io Revisited

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10484850" target="_blank" >RIV/00216208:11320/24:10484850 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=p7zqXRSvSU" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=p7zqXRSvSU</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1029/2023GL107869" target="_blank" >10.1029/2023GL107869</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Tidal Heating in a Subsurface Magma Ocean on Io Revisited

Popis výsledku v původním jazyce

We investigate the tidal dissipation in Io&apos;s hypothetical fluid magma ocean using a new approach based on the solution of the 3D Navier-Stokes equations. Our results indicate that the presence of a shallow magma ocean on top of a solid, partially molten layer leads to an order of magnitude increase in dissipation at low latitudes. Tidal heating in Io&apos;s magma ocean does not correlate with the distribution of hot spots, and is maximum for an ocean thickness of about 1 km and a viscosity of less than 104 Pa s. Due to the Coriolis effect, the k2 Love number can depend on the harmonic order. We show that the analysis of k2 may not reveal the presence of a fluid magma ocean if the ocean thickness is less than 2 km. If the fluid layer is thicker than 2 km, k20 approximate to k22/2 approximate to 0.7. Jupiter&apos;s moon Io is the most active volcanic body in the Solar System. Although it is generally accepted that Io&apos;s volcanic activity is driven by the heat generated by tidal friction, the origin and the distribution of tidal heating within Io&apos;s interior remain a subject of debate. Here we investigate the tidal dissipation in Io&apos;s hypothetical fluid magma ocean using a new approach based on the solution of general equations describing the motion of viscous fluid. Our results indicate that the presence of a shallow magma ocean on top of a solid, partially molten layer leads to an order of magnitude increase in dissipation at low latitudes. Tidal heating in Io&apos;s magma ocean does not correlate with the distribution of hot spots, and is maximum for an ocean thickness of about 1 km and a viscosity of less than 104 Pa s. We also discuss the sensitivity of Io&apos;s gravity signature to the presence of a magma ocean and provide estimates of gravitational perturbations induced by tidal deformation. The presence of a shallow magma ocean on top of a partially molten layer leads to a strong increase in tidal dissipation at low latitudes Due to the Coriolis effect, the degree-2 Love numbers for models with a magma ocean can depend on the harmonic order The tidal Love numbers are not sensitive to the presence of a fluid magma ocean if the thickness of the fluid layer is less than 2 km

Název v anglickém jazyce

Tidal Heating in a Subsurface Magma Ocean on Io Revisited

Popis výsledku anglicky

We investigate the tidal dissipation in Io&apos;s hypothetical fluid magma ocean using a new approach based on the solution of the 3D Navier-Stokes equations. Our results indicate that the presence of a shallow magma ocean on top of a solid, partially molten layer leads to an order of magnitude increase in dissipation at low latitudes. Tidal heating in Io&apos;s magma ocean does not correlate with the distribution of hot spots, and is maximum for an ocean thickness of about 1 km and a viscosity of less than 104 Pa s. Due to the Coriolis effect, the k2 Love number can depend on the harmonic order. We show that the analysis of k2 may not reveal the presence of a fluid magma ocean if the ocean thickness is less than 2 km. If the fluid layer is thicker than 2 km, k20 approximate to k22/2 approximate to 0.7. Jupiter&apos;s moon Io is the most active volcanic body in the Solar System. Although it is generally accepted that Io&apos;s volcanic activity is driven by the heat generated by tidal friction, the origin and the distribution of tidal heating within Io&apos;s interior remain a subject of debate. Here we investigate the tidal dissipation in Io&apos;s hypothetical fluid magma ocean using a new approach based on the solution of general equations describing the motion of viscous fluid. Our results indicate that the presence of a shallow magma ocean on top of a solid, partially molten layer leads to an order of magnitude increase in dissipation at low latitudes. Tidal heating in Io&apos;s magma ocean does not correlate with the distribution of hot spots, and is maximum for an ocean thickness of about 1 km and a viscosity of less than 104 Pa s. We also discuss the sensitivity of Io&apos;s gravity signature to the presence of a magma ocean and provide estimates of gravitational perturbations induced by tidal deformation. The presence of a shallow magma ocean on top of a partially molten layer leads to a strong increase in tidal dissipation at low latitudes Due to the Coriolis effect, the degree-2 Love numbers for models with a magma ocean can depend on the harmonic order The tidal Love numbers are not sensitive to the presence of a fluid magma ocean if the thickness of the fluid layer is less than 2 km

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10500 - Earth and related environmental sciences

Projekt

—

Návaznosti

S - Specificky vyzkum na vysokych skolach

Rok uplatnění

2024

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Geophysical Research Letters

ISSN

0094-8276

e-ISSN

1944-8007

Svazek periodika

51

Číslo periodika v rámci svazku

10

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

10

Strana od-do

e2023GL107869

Kód UT WoS článku

001219662700001

EID výsledku v databázi Scopus

2-s2.0-85192915429