Observational constraints on the identification and distribution of chaotic terrain on icy satellites

Neish, C. D.; Prockter, L. M.; Patterson, G. W.

doi:10.1016/j.icarus.2012.07.009

Cited by 10 publications

(4 citation statements)

References 19 publications

(54 reference statements)

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“…Their similar sizes suggest that they may have a common origin and the different surface morphologies record different stages in the evolution of a single event within the ice shell (e.g., Pappalardo et al, 1998, Greenberg et al, 1999, Collins and Nimmo, 2009. Lenticulae and larger chaos features are abundant with large spatial variability in number density (Neish et al, 2012) and type (Culha and Manga, 2016), and they cover approximately 5% to 40% of the surface (Figueredo andGreeley, 2004, Riley et al, 2000). Lenticulae have attracted attention because their formation should provide insights into heat and mass transport processes within Europa's ice shell (e.g., Quick and Marsh, 2016), including possible liquid water transport from the underlying ocean to the surface and near-surface of the ice shell.…”

Section: Introductionmentioning

confidence: 99%

Formation of lenticulae on Europa by saucer-shaped sills

Manga

Michaut

2017

Icarus

106

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Section: Introductionmentioning

confidence: 99%

Formation of lenticulae on Europa by saucer-shaped sills

Manga

Michaut

2017

Icarus

106

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“…18) using thermal images with resolutions as low as 6 km/pixel laid over visible imaging data [19,38]. Chaotic features and tectonic terrain on Europa can also be characterized with thermal images on the scale of a few kilometers [44,45]. The thermal radiometer concept presented here is able to obtain thermal images of Europa's surface at scales of ≤1 km/pixel to supplement visible context images and thereby allow any sites of current or recent activity to be linked to their source structures on the surface (Fig.…”

Section: Characterizing Compelling Landing Sites With Anomalous Tempementioning

confidence: 99%

Dual-telescope multi-channel thermal-infrared radiometer for outer planet fly-by missions

et al. 2016

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The design of a versatile dual-telescope thermal-infrared radiometer spanning the spectral wavelength range 8 to 200 µm, in five spectral pass bands, for outer planet fly-by missions is described. The dual-telescope design switches between a narrow-field-of-view and a wide-field-of-view to provide optimal spatial resolution images within a range of spacecraft encounters to the target. The switchable dual-field-of-view system uses an optical configuration based on the axial rotation of a source-select mirror along the optical axis. The optical design, spectral performance, radiometric accuracy, and retrieval estimates of the instrument are discussed. This is followed by an assessment of the surface coverage performance at various spatial resolutions by using the planned NASA Europa Mission 13-F7 fly-by trajectories as a case study.

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“…Chaos terrain-regions in which pre-existing terrain is broken into plates sitting in a lower-albedo hummocky matrix material (Carr et al 1998;Greeley et al 1998)-is likely part of the newest epoch in resurfacing processes on Europa (Riley et al 2000;Figueredo & Greeley 2004;Neish et al 2012;Leonard et al 2018). Chaos has a relatively large size range, from ∼5 km to >100 km in diameter (Figueredo & Greeley 2003;Noviello et al 2019;Singer et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Stable Brine Layers beneath Europa’s Chaos

Chivers,

Buffo,

Schmidt

2023

Planet. Sci. J.

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The formation mechanism of Europa’s large chaos terrain (>∼100 km diameter) and associated lenticulae (<∼10 km diameter) has been debated since their observations by the Galileo spacecraft. Their geomorphology and distribution suggest there may be reservoirs of saline liquid water 1–3 km beneath the surface—the “shallow water” model—generated by injection of ocean water or melting of the ice shell. Recent investigations on the evolution of small shallow-water bodies (≤103 km3) suggests that salts with a small effect on melting point (MgSO4) can extend the lifetime of saline bodies by ∼5% compared to freshwater reservoirs. However, sodium chloride, identified as a potential oceanic salt, has a significantly stronger impact on the freezing point, suggesting a further extension of liquid lifetimes. Moreover, the substantial volumes of liquid water (∼104 km3) beneath large chaos could be melted in situ rather than injected through a fracture, implying a distinct chemistry and formation environment. Here, we use numerical models to explore how the chemistry and disparate origins of shallow water control its evolution and lifetime. For small, injected sills, we find that NaCl can extend their liquid lifetime to ∼140 kyr—up to a ∼60% increase over freshwater sills. Saline melt lenses will last at least 175 kyr but, in contrast to sills, may persist as a stable layer of brine beneath the surface for over 500 kyr. Our results provide further support for the presence of liquid water at shallow depths within Europa’s ice shell today.

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Observational constraints on the identification and distribution of chaotic terrain on icy satellites

Cited by 10 publications

References 19 publications

Formation of lenticulae on Europa by saucer-shaped sills

Formation of lenticulae on Europa by saucer-shaped sills

Dual-telescope multi-channel thermal-infrared radiometer for outer planet fly-by missions

Stable Brine Layers beneath Europa’s Chaos

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