Melting in High-Pressure Ice Layers of Large Ocean Worlds-Implications for Volatiles Transport

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10384960" target="_blank" >RIV/00216208:11320/18:10384960 - isvavai.cz</a>

Result on the web

<a href="https://doi.org/10.1029/2018GL078889" target="_blank" >https://doi.org/10.1029/2018GL078889</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1029/2018GL078889" target="_blank" >10.1029/2018GL078889</a>

Result language

angličtina

Original language name

Melting in High-Pressure Ice Layers of Large Ocean Worlds-Implications for Volatiles Transport

Original language description

A high-pressure ice layer controls the exchange of heat and material between the silicate core and the ocean of Ganymede and Titan. We have shown (Kalousova et al., 2018, ) that a temperate (partially molten) layer is always present at the ocean interface. Another temperate layer with a few percent of water may be present at the silicates interface for low values of Rayleigh number. We derive scaling laws to predict the critical value under which this temperate layer exists and the amount of generated melt. The presence of liquid water in contact with silicates was probably limited to the early history, providing a pathway for the transfer of salts and volatiles like Ar-40 to the ocean. We also derive scaling laws for the water outflow velocity and for the top temperate layer thickness. These laws can be used to model the global thermal and compositional evolution of large ocean worlds. Plain Language Summary Ocean worlds, where a deep global ocean is present below the icy crust, provide an interesting habitable environment where life may exist. On Enceladus, which is small, and Europa, where the H2O/silicate (water/rock) ratio is small, the global ocean is in direct contact with the silicates. On Titan and Ganymede, where this ratio is large, a layer of high-pressure (HP) ice is present between the ocean and the rocky core. This paper shows that early in their evolution, the lower part of this HP ice layer was temperate (porous ice with water in the pores). Such a temperate layer enables a silicates-ocean exchange of salts and volatiles such as Ar-40 that was measured in Titan&apos;s atmosphere by the Cassini mission. It also provides a potentially habitable environment in Ganymede, the largest moon in the solar system that will be studied by the ESA JUICE mission.

Czech name

—

Czech description

—

Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10500 - Earth and related environmental sciences

Project

—

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2018

Confidentiality

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

Name of the periodical

Geophysical Research Letters

ISSN

0094-8276

e-ISSN

—

Volume of the periodical

45

Issue of the periodical within the volume

16

Country of publishing house

US - UNITED STATES

Number of pages

8

Pages from-to

8096-8103

UT code for WoS article

000445612500025

EID of the result in the Scopus database

2-s2.0-85053137639