Timing of water plume eruptions on Enceladus explained by interior viscosity structure

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F15%3A10314657" target="_blank" >RIV/00216208:11320/15:10314657 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1038/NGEO2475" target="_blank" >http://dx.doi.org/10.1038/NGEO2475</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1038/NGEO2475" target="_blank" >10.1038/NGEO2475</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Timing of water plume eruptions on Enceladus explained by interior viscosity structure

Popis výsledku v původním jazyce

At the south pole of Saturn's icy moon Enceladus, eruptions of water vapour and ice emanate from warm tectonic ridges(1-4). Observations in the infrared(5) and visible(6) spectra have shown an orbital modulation of the plume brightness, which suggests that the eruption activity is influenced by tidal forces. However, the observed activity seems to be delayed by several hours with respect to predictions based on simple tidal models(6,7). Here we simulate the viscoelastic tidal response of Enceladus witha full three-dimensional numerical model(8,9) and show that the delay in eruption activity may be a natural consequence of the viscosity structure in the south-polar region and the size of the putative subsurface ocean. By systematically comparing simulations of variations in normal stress along faults with plume brightness data, we show that the observed activity is reproduced for two classes of interior models with contrasting thermal histories: a low-viscosity convective region above

Název v anglickém jazyce

Timing of water plume eruptions on Enceladus explained by interior viscosity structure

Popis výsledku anglicky

At the south pole of Saturn's icy moon Enceladus, eruptions of water vapour and ice emanate from warm tectonic ridges(1-4). Observations in the infrared(5) and visible(6) spectra have shown an orbital modulation of the plume brightness, which suggests that the eruption activity is influenced by tidal forces. However, the observed activity seems to be delayed by several hours with respect to predictions based on simple tidal models(6,7). Here we simulate the viscoelastic tidal response of Enceladus witha full three-dimensional numerical model(8,9) and show that the delay in eruption activity may be a natural consequence of the viscosity structure in the south-polar region and the size of the putative subsurface ocean. By systematically comparing simulations of variations in normal stress along faults with plume brightness data, we show that the observed activity is reproduced for two classes of interior models with contrasting thermal histories: a low-viscosity convective region above

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

DE - Zemský magnetismus, geodesie, geografie

OECD FORD obor

—

Projekt

<a href="/cs/project/GA14-04145S" target="_blank" >GA14-04145S: Vnitřní vývoj krátkoperiodických terestrických exoplanet</a><br>

Návaznosti

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

Rok uplatnění

2015

Kód důvěrnosti údajů

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

Název periodika

Nature Geoscience

ISSN

1752-0894

e-ISSN

—

Svazek periodika

8

Číslo periodika v rámci svazku

8

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

4

Strana od-do

601-604

Kód UT WoS článku

000358735500011

EID výsledku v databázi Scopus

2-s2.0-84938587376