Solid tidal friction above a liquid water reservoir as the origin of the south pole hotspot on Enceladus

Tobie, G.; Čadek, O.; Sotin, C.

doi:10.1016/j.icarus.2008.03.008

Cited by 126 publications

(156 citation statements)

References 48 publications

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“…The presence of a liquid water reservoir is also supported by the gravity measurements performed by Cassini (Iess et al, 2014), as well as by models of tidal deformation (e.g. Nimmo et al, 2007;Tobie et al, 2008) ( Fig. 4d).…”

Section: Evidence For Subsurface Salt-water Reservoirs On Enceladussupporting

confidence: 55%

Science goals and mission concept for the future exploration of Titan and Enceladus

Tobie¹,

Teanby²,

Coustenis³

et al. 2014

Planetary and Space Science

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Saturn's moons, Titan and Enceladus, are two of the Solar System's most enigmatic bodies and are prime targets for future space exploration. Titan provides an analogue for many processes relevant to the Earth, more generally to outer Solar System bodies, and a growing host of newly discovered icy exoplanets. Processes represented include: atmospheric dynamics, complex organic chemistry, meteorological cycles (with methane as a working fluid), astrobiology, surface liquids and lakes, geology, fluvial and aeolian erosion, and interactions with an external plasma environment. In addition, exploring Enceladus over multiple targeted flybys will give us a unique opportunity to further study the most active icy moon in our Solar System as revealed by Cassini and to analyse in situ its active plume with highly capable instrumentation addressing its complex chemistry and dynamics. Enceladus' plume likely represents the most accessible samples from an extra-terrestrial liquid water environment in the Solar system, which has far reaching implications for many areas of planetary and biological science. Titan with its massive atmosphere and Enceladus with its active plume are prime planetary objects in the Outer Solar System to perform in situ investigations. In the present paper, we describe the science goals and key measurements to be

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Section: Evidence For Subsurface Salt-water Reservoirs On Enceladussupporting

confidence: 55%

Science goals and mission concept for the future exploration of Titan and Enceladus

Tobie¹,

Teanby²,

Coustenis³

et al. 2014

Planetary and Space Science

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“…[10] Such a thinning of the ice shell could be related to enhanced heat flow from the rocky core, as in the ''south polar sea'' hypothesis of Collins and Goodman [2007], but given the low likelihood of any substantial heat flow from the core, even tidal heat flow [Roberts and Nimmo, 2008], a more plausible idea is that tidal heating in the deeper levels of the ice shell itself has led to ice melting and drainage, and shell thinning [e.g., Tobie et al, 2008].…”

Section: à2mentioning

confidence: 99%

One‐hundred‐km‐scale basins on Enceladus: Evidence for an active ice shell

Schenk

McKinnon²

2009

Geophysical Research Letters

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Stereo‐derived topographic mapping of ∼50% of Enceladus reveals at least 6 large‐scale, ovoid depressions (basins) 90–175 km across and 800‐to‐1500 m deep and uncorrelated with geologic boundaries. In contrast, the south polar depression is larger and apparently shallower and correlates with active resurfacing. The shape and scale of the basins is inconsistent with impact, geoid surface deflections, or with dynamically supported topography. Isostatic thinning of Enceladus' ice shell associated with upwellings (and tidally‐driven ice melting) can plausibly account for these basins. Thinning implies upwarping of the base of the shell of ∼10–20 km beneath the depressions, depending on total shell thickness; loss of near‐surface porosity due to enhanced heat flow may also contribute to basin lows. Alternatively, the basins may overly cold, inactive, and hence denser ice, but thermal isostasy alone requires thermal expansion more consistent with clathrate hydrate than water ice.

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“…It has been suggested that the tidal strain in icy satellites is so small that the response of the object is non-linear (Montagnat and Duval 2004). The situation may be different in the case of Enceladus and Europa, subject to stresses greater than 0.1 MPa and possible stress concentration, as suggested by the model of Tobie et al (2008). Also, satellites' orbital properties have evolved as a consequence of the tides they are subject to and the tides they exert on their primaries.…”

Section: Mechanisms Driving Dissipation In Icy Satellitesmentioning

confidence: 99%