A comprehensive dataset for the thermal conductivity of ice Ih for application to planetary ice shells

Wolfenbarger, Natalie S.; Carnahan, Evan; Jordan, Jacob S.; Hesse, M. A.

doi:10.1016/j.dib.2021.107079

Cited by 4 publications

(6 citation statements)

References 9 publications

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“…In the literature, numerous fitting adjustments for the experimental thermal conductivity data have been found, such as the one used by Andersson & Inaba ( 2005 ), k = a / T + b + c • T , Slack ( 1980 ), k = a / T , or linear fitting (Bonales et al 2017 , and references therein). Ho we ver, in all these cited cases, the thermal conductivity data are for pure H 2 O ice (Andersson 2018 ;Wolfenbarger et al 2021 ).…”

Section: Magnesium Chloride (Mgcl 2 ) Solutionmentioning

confidence: 95%

Thermal conductivity measurements of macroscopic frozen salt ice analogues of Jovian icy moons in support of the planned JUICE mission

Díaz

Aparicio

Caro

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The study of thermal properties of frozen salt solutions representative of ice layers in Jovian moons is crucial to support the JUpiter ICy moons Explorer (JUICE) (ESA) and Europa Clipper (NASA) missions, which will be launched in the upcoming years to make detailed observations of the giant gaseous planet Jupiter and three of its largest moons (Ganymede, Europa, and Callisto), due to the scarcity of experimental measurements. Therefore, we have conducted a set of experiments to measure and study the thermal conductivity of macroscopic frozen salt solutions of particular interest in these regions, including sodium chloride (NaCl), magnesium sulphate (MgSO4), sodium sulphate (Na2SO4), and magnesium chloride (MgCl2). Measurements were performed at atmospheric pressure and temperatures from 0 to -70○C in a climatic chamber. Temperature and calorimetry were measured during the course of the experiments. An interesting side effect of these measurements is that they served to spot phase changes in the frozen salt solutions, even for very low salt concentrations. A small sample of the liquid salt-water solution was set aside for the calorimetry measurements. These experiments and the measurements of thermal conductivity and calorimetry will be valuable to constrain the chemical composition, physical state, and temperature of the icy crusts of Ganymede, Europa, and Callisto.

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Section: Magnesium Chloride (Mgcl 2 ) Solutionmentioning

confidence: 95%

Thermal conductivity measurements of macroscopic frozen salt ice analogues of Jovian icy moons in support of the planned JUICE mission

Díaz

Aparicio

Caro

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Methane clathrates affect the convective dynamics of an ice shell because they have higher viscosity (Durham et al., 2003; Goldsby & Kohlstedt, 2001), lower thermal conductivity (Carnahan et al., 2021; Sloan & Koh, 2007; Wolfenbarger et al., 2021), and higher density (Feistel & Wagner, 2006; Helgerud et al., 2009) than water ice (Figures 2a–2c). The physical properties of methane clathrates and ice are pressure and temperature dependent.…”

Section: Methodsmentioning

confidence: 99%

Dynamics of Mixed Clathrate‐Ice Shells on Ocean Worlds

Carnahan

Vance

Hesse

et al. 2022

Geophysical Research Letters

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The habitability of oceans within icy worlds depends on material and heat transport through their outer ice shells. Previous work shows a methane clathrate layer at the upper surface of the ice shell of Titan thickens the convecting region, while on Pluto a clathrate layer at the base of the ice shell hinders convection. In this way, the dynamics of clathrate‐ice shells may be essential to the thermal evolution and habitability of ocean worlds. However, studies to date have not addressed the dynamics that determine the location of clathrates within the ice shell. Here, we show that, in contrast to previous studies, clathrates accumulating at the base of the ice shell are entrained throughout the shell. Clathrates are stiffer than ice. As a result, entrainment slows convection and thickens the conductive lid across a range of ocean worlds, potentially preserving sub‐ice oceans but limiting avenues for material transport into them.

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“…where q is the upward heat flux passing through a spherical surface at radius r and k is the thermal conductivity at that surface. The thermal conductivity of ice layers is assumed to follow a k ∼ 1/T dependence (e.g., Wolfenbarger et al, 2021). If we further assume q, local gravitational acceleration g, and layer mass density ρ are approximately constant throughout the ice shell, Equation 1yields In Equation 2, subscripts "bot" and "top" refer to pressures P and temperatures T at the bottom and top of the ice shell, respectively.…”

Section: Initial Ice Shell Thermal Profilementioning

confidence: 99%

“…To start, the ice shell properties are calculated from the ice Ih EOS implemented by SeaFreeze assuming a conductive thermal profile with the Fourier heat law (Turcotte & Schubert, 2002):

q=-k\frac{\partial T}{\partial r},

where q is the upward heat flux passing through a spherical surface at radius r and k is the thermal conductivity at that surface. The thermal conductivity of ice layers is assumed to follow a k ∼ 1/ T dependence (e.g., Wolfenbarger et al., 2021). If we further assume q , local gravitational acceleration g , and layer mass density ρ are approximately constant throughout the ice shell, Equation yields

T(P)={T}_{\mathrm{b}\mathrm{o}\mathrm{t}}^{\tfrac{P-{P}_{\mathrm{t}\mathrm{o}\mathrm{p}}}{{P}_{\mathrm{b}\mathrm{o}\mathrm{t}}-{P}_{\mathrm{t}\mathrm{o}\mathrm{p}}}}{T}_{\mathrm{t}\mathrm{o}\mathrm{p}}^{\tfrac{{P}_{\mathrm{b}\mathrm{o}\mathrm{t}}-P}{{P}_{\mathrm{b}\mathrm{o}\mathrm{t}}-{P}_{\mathrm{t}\mathrm{o}\mathrm{p}}}}.

…”

Section: Self‐consistent Model Designmentioning

confidence: 99%

“…In PlanetProfile, except where top or bottom values are specified, we evaluate physical properties at the midpoint in pressure ((P surf + P b )/2) and at the convecting temperature after Solomatov (1995). We use expressions for ice thermal conductivity based on best-fit models from Wolfenbarger et al (2021) for ice Ih and Andersson and Inaba (2005) for other ice phases.…”

Section: Ice Shell Convectionmentioning

confidence: 99%

See 1 more Smart Citation

PlanetProfile: Self‐Consistent Interior Structure Modeling for Ocean Worlds and Rocky Dwarf Planets in Python

Styczinski,

Vance,

Melwani Daswani

2023

Earth and Space Science

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The open‐source PlanetProfile framework was developed to investigate the interior structure of icy moons based on collectively matching their observed properties and comparative planetology. The software relates observed and measured properties, assumptions such as the type of materials present, and laboratory equation‐of‐state (EOS) data through geophysical and thermodynamic models to evaluate radial profiles of mechanical, thermodynamic, and electrical properties, as self‐consistently as possible. We have created a Python version of PlanetProfile. In the process, we have made optimization improvements and added parallelization and parameter‐space search features to utilize fast operation for investigating unresolved questions in planetary geophysics, in which many model inputs are poorly constrained. The Python version links to other scientific software packages, including for evaluating EOS data, magnetic induction calculations, and seismic calculations. Physical models in PlanetProfile have been reconfigured to improve self‐consistency and generate the most realistic relationships between properties. In this work, we focus on the description of the software design and algorithms in detail, summarize model results for major moons across the outer solar system, and discuss new inferences about the interior structure of several bodies. The high values and narrow uncertainty ranges reported for the axial moments of inertia for Callisto, Titan, and Io are difficult to reconcile with the realistic physical and chemical approximations applied, requiring highly porous rock layers equivalent to incomplete differentiation for Callisto and Titan, and a high rock melt fraction for Io. Radial profiles for each model and comparison to prior work are provided as Zenodo archives.

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A comprehensive dataset for the thermal conductivity of ice Ih for application to planetary ice shells

Cited by 4 publications

References 9 publications

Thermal conductivity measurements of macroscopic frozen salt ice analogues of Jovian icy moons in support of the planned JUICE mission

Thermal conductivity measurements of macroscopic frozen salt ice analogues of Jovian icy moons in support of the planned JUICE mission

Dynamics of Mixed Clathrate‐Ice Shells on Ocean Worlds

PlanetProfile: Self‐Consistent Interior Structure Modeling for Ocean Worlds and Rocky Dwarf Planets in Python

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