Inferring Io's interior from tidal monitoring

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10452105" target="_blank" >RIV/00216208:11320/22:10452105 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=vv3ynWJMdg" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=vv3ynWJMdg</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.icarus.2021.114737" target="_blank" >10.1016/j.icarus.2021.114737</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Inferring Io's interior from tidal monitoring

Popis výsledku v původním jazyce

Io&apos;s spectacular volcanic activity involves strong tidal dissipation in its interior. Magnetic induction measurements and surface observations of the volcanic activity indicate the presence of significant melt in the interior, but the melt distribution remains unconstrained. Tidal deformation of a planetary body is strongly related to the rheological properties of the interior, and thus, to a larger extent, to the melt content. The amplitude of tidal deformation may be monitored by future missions from spacecraft tracking, altimetry and high-resolution imaging, giving access to the potential and displacement Love numbers k(2), h(2) and l(2). To anticipate such measurements, we compute the tidal response described by both shear and bulk viscoelastic rheology for various rheological properties and distributions of melt within Io&apos;s interior. We show that the distribution of tidal heating between the mantle and the asthenosphere is very sensitive to the assumed melt fraction in the asthenosphere. For melt fraction smaller that a critical value called rheological critical melt fraction (phi(c)), corresponding to a transition from solid-dominated behavior to liquid-dominated one, the dissipation is mostly occurring in the mantle. For this mantle-dominated regime, a viscosity of the solid rock matrix smaller than 10(17)-10(18) Pa s is required to reproduce the estimated heat output (ranging between 65 and 125 TW). For melt fraction slightly above phi(c) dissipation mostly occurs in the asthenosphere, resulting in a radical change of dissipation pattern characterized by a reduction of polar contribution. Despite this clear transition, changes in terms of Love numbers k(2), h(2) and l(2) are subtle and would require high precision measurements. k(2) is only slightly sensitive to the melt distribution and is mainly sensitive to the density of the metallic core, with a Love number potentially as high as 0.1 for a low density core and below 0.06 for a high density core. h(2) and especially l(2) are more sensitive to the melt distribution, with a clear distinction between mantle-dominated and asthenosphere-dominated regimes, difference that is amplified by the contribution of bulk viscoelastic response. The combined detection of high h(2) (&gt; 0.2) and l(2) (&gt; 0.07) values and a low k(2) (&lt; 0.1) would be confirmation that bulk dissipation plays a crucial role in the heat budget of Io and will provide constraints on the thickness (&lt; 100 km) and melt fraction (&gt; phi(c)) of the partially molten asthenosphere. Accurate determination of Love numbers, combined with libration and magnetic induction measurement may provide crucial constraints on the melt profile in Io&apos;s interior.

Název v anglickém jazyce

Inferring Io's interior from tidal monitoring

Popis výsledku anglicky

Io&apos;s spectacular volcanic activity involves strong tidal dissipation in its interior. Magnetic induction measurements and surface observations of the volcanic activity indicate the presence of significant melt in the interior, but the melt distribution remains unconstrained. Tidal deformation of a planetary body is strongly related to the rheological properties of the interior, and thus, to a larger extent, to the melt content. The amplitude of tidal deformation may be monitored by future missions from spacecraft tracking, altimetry and high-resolution imaging, giving access to the potential and displacement Love numbers k(2), h(2) and l(2). To anticipate such measurements, we compute the tidal response described by both shear and bulk viscoelastic rheology for various rheological properties and distributions of melt within Io&apos;s interior. We show that the distribution of tidal heating between the mantle and the asthenosphere is very sensitive to the assumed melt fraction in the asthenosphere. For melt fraction smaller that a critical value called rheological critical melt fraction (phi(c)), corresponding to a transition from solid-dominated behavior to liquid-dominated one, the dissipation is mostly occurring in the mantle. For this mantle-dominated regime, a viscosity of the solid rock matrix smaller than 10(17)-10(18) Pa s is required to reproduce the estimated heat output (ranging between 65 and 125 TW). For melt fraction slightly above phi(c) dissipation mostly occurs in the asthenosphere, resulting in a radical change of dissipation pattern characterized by a reduction of polar contribution. Despite this clear transition, changes in terms of Love numbers k(2), h(2) and l(2) are subtle and would require high precision measurements. k(2) is only slightly sensitive to the melt distribution and is mainly sensitive to the density of the metallic core, with a Love number potentially as high as 0.1 for a low density core and below 0.06 for a high density core. h(2) and especially l(2) are more sensitive to the melt distribution, with a clear distinction between mantle-dominated and asthenosphere-dominated regimes, difference that is amplified by the contribution of bulk viscoelastic response. The combined detection of high h(2) (&gt; 0.2) and l(2) (&gt; 0.07) values and a low k(2) (&lt; 0.1) would be confirmation that bulk dissipation plays a crucial role in the heat budget of Io and will provide constraints on the thickness (&lt; 100 km) and melt fraction (&gt; phi(c)) of the partially molten asthenosphere. Accurate determination of Love numbers, combined with libration and magnetic induction measurement may provide crucial constraints on the melt profile in Io&apos;s interior.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10500 - Earth and related environmental sciences

Projekt

<a href="/cs/project/GA19-10809S" target="_blank" >GA19-10809S: Termomechanické procesy v ledových měsících z pohledu numerického modelování</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2022

Kód důvěrnosti údajů

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

Název periodika

Icarus

ISSN

0019-1035

e-ISSN

1090-2643

Svazek periodika

373

Číslo periodika v rámci svazku

January

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

12

Strana od-do

114737

Kód UT WoS článku

000726937800006

EID výsledku v databázi Scopus

2-s2.0-85119965552