The temperature and width of an active fissure on Enceladus measured with Cassini VIMS during the 14 April 2012 South Pole flyover

Goguen, J. D.; Buratti, B. J.; Brown, R. H.; Clark, R. N.; Nicholson, P.; Hedman, M. M.; Howell, R. R.; Sotin, C.; Cruikshank, D. P.; Baines, K. H.; Lawrence, K.; Spencer, J. R.; Blackburn, D. G.

doi:10.1016/j.icarus.2013.07.012

Cited by 76 publications

(72 citation statements)

References 26 publications

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“…The vents themselves are estimated to be only on the order of 9 m in width on the basis of VIMS thermal data for one particular example on Baghdad Sulcus (Goguen et al 2013). The vent width is comparable to the smallest ice blocks visible in our highest-resolution Cassini images.…”

Section: Correlation Of Geysers With Unique Morphological Featuresmentioning

confidence: 67%

“…It might also be possible for adjacent vents to merge into a single one by propagation and enlargement of cracks connecting them. Goguen et al (2013) estimate that vents detected in Cassini VIMS thermal observations of Baghdad Sulcus has an orifice diameter on the order of 9 m in width-a size that is generally below the best spatial resolutions of our Imaging Science Subsystem (ISS) Narrow Angle Camera (NAC) imaging coverage.…”

Section: Introductionmentioning

confidence: 93%

“…Local sculpting of the surface through sublimation-aided erosion or ablation of surface ices by the jet may be enhanced in the vicinity of an active geyser (cf. Goguen et al 2013). Finally, a build-up of spattered or cold-trapped ice could accrete around the vent to form circum-eruption ramps, pedestals or bench-like formations that may flank the vent.…”

Section: Correlation Of Geysers With Unique Morphological Featuresmentioning

confidence: 99%

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Enceladus’ Geysers: Relation to Geological Features

Helfenstein

Porco

2015

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We apply histogram analysis, photogeological methods, and tidal stress modeling to Porco et al.ʼs survey of 101 Enceladus South Polar Basin geysers and their three-dimensional orientations to test if the jet azimuths are influenced by their placement relative to surface morphology and tectonic structures. Geysers emplaced along the three most active tiger stripe fractures (Damascus Sulcus, Baghdad Sulcus, and Cairo Sulcus) occur in local groupings with relatively uniform nearest-neighbor separation distances (∼5 km). Their placement may be controlled by uniformly spaced en echelon Riedel-type shear cracks originating from left-lateral strike-slip fault motion inferred to occur along tiger stripes. The spacing would imply a lithosphere thickness of ∼5 km in the vicinity of the tiger stripes. The orientations of tilted geyser jets are not randomly distributed; rather their azimuths correlate with the directions either of tiger stripes, cross-cutting fractures, or else fine-scale local tectonic fabrics. Diurnal tidal stress modeling suggests that periodic changes of plume activity are significantly affected by crosscutting fractures that open and close at different times than the tiger stripes that they intersect. We find evidence of sub-kilometer scale morphological modification of surface geological features surrounding geysers from sublimation-aided erosion, and ablation, and scouring. We propose that the simultaneous crushing and shearing action of periodic transpressional tidal stress on ice condensing on the inside walls of geyser conduits is the mechanism that extrudes the peculiar, paired narrow ridges known as "shark fins" that flank the medial tiger stripe fissures. We present a gallery of high-resolution image mosaics showing the placement of all the jets in their source region and consequently their geological context.

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Section: Correlation Of Geysers With Unique Morphological Featuresmentioning

confidence: 67%

Section: Introductionmentioning

confidence: 93%

Section: Correlation Of Geysers With Unique Morphological Featuresmentioning

confidence: 99%

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Enceladus’ Geysers: Relation to Geological Features

Helfenstein

Porco

2015

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“…Figure 7 compares these timescales for various crack widths D. Despite the roughness and uncertainties of the above analysis, the large range of ascent and freezing timescales involved entail a specific threshold crack width, of order 1 m, for successful ascent. It is worth noting that the width of a fracture on Enceladus has recently been estimated at 9 m (Goguen et al, 2013).…”

Section: Freezing During Ascentmentioning

confidence: 99%

Prerequisites for explosive cryovolcanism on dwarf planet-class Kuiper belt objects

Neveu

Desch

Shock

et al. 2015

Icarus

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Explosive extrusion of cold material from the interior of icy bodies, or cryovolcanism, has been observed on Enceladus and, perhaps, Europa, Triton, and Ceres. It may explain the observed evidence for a young surface on Charon (Pluto's surface is masked by frosts). Here, we evaluate prerequisites for cryovolcanism on dwarf planet-class Kuiper belt objects (KBOs). We first review the likely spatial and temporal extent of subsurface liquid, proposed mechanisms to overcome the negative buoyancy of liquid water in ice, and the volatile inventory of KBOs. We then present a new geochemical equilibrium model for volatile exsolution and its ability to drive upward crack propagation. This novel approach bridges geophysics and geochemistry, and extends geochemical modeling to the seldom-explored realm of liquid water at subzero temperatures. We show that carbon monoxide (CO) is a key volatile for gas-driven fluid ascent; whereas CO 2 and sulfur gases only play a minor role. N 2 , CH 4 , and H 2 exsolution may also drive explosive cryovolcanism if hydrothermal activity produces these species in large amounts (a few percent with respect to water). Another important control on crack propagation is the internal structure: a hydrated core makes explosive cryovolcanism easier, but an undifferentiated crust does not. We briefly discuss other controls on ascent such as fluid freezing on crack walls, and outline theoretical advances necessary to better understand cryovolcanic processes. Finally, we make testable predictions for the 2015 New Horizons flyby of the Pluto-Charon system.

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“…5 This observation presented a strong challenge to the single-component liquid water model because gases in this abundance cannot be dissolved into liquid water. The highest temperature reported at that time was 145 ± 14 K, and as of the latest measurements, it is 197 ± 20 K (taken in 2012 and reported in Goguen et al 2013). 5 Estimates of the composition of the plume have been revised several times.…”

Section: A Time For Consolidation Then Triton and Enceladusmentioning

confidence: 98%