The geology of Hotei Regio, Titan: Correlation of Cassini VIMS and RADAR

Soderblom, Laurence A.; Brown, R. H.; Soderblom, Jason M.; Barnes, Jason W.; Kirk, Randolph L.; Sotin, C.; Jaumann, R.; Mackinnon, D. J.; Mackowski, Daniel W.; Baines, K. H.; Buratti, B. J.; Clark, R. N.; Nicholson, P. D.

doi:10.1016/j.icarus.2009.07.033

Cited by 64 publications

(77 citation statements)

References 47 publications

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“…These morphologies include "smooth and/or sparsely cratered surfaces, infilled craters and graben, domes, lobate features, ridges, calderalike features, and low-albedo surfaces" (Fagents, 2003). Recently, similar morphologies have been studied on Titan using Cassini radar and infrared imagery (Lopes et al, 2007;Wall et al, 2009;Le Corre et al, 2009;Soderblom et al, 2009). To assess the possible cryovolcanic origin of these observed morphologies, laboratory experiments and modeling studies have investigated the rheological properties of cryolavas of watervolatile compositions (Schenk, 1991;Kargel et al, 1991;Zhong et al, 2009).…”

Section: Evidence For Cryovolcanism In the Outer Solar Systemmentioning

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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Section: Evidence For Cryovolcanism In the Outer Solar Systemmentioning

confidence: 99%

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

Neveu

Desch

Shock

et al. 2015

Icarus

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“…Applying an updated version of the same model, McCord et al (2006) found portions of Titan's surface consistent with a ''dirty water ice'' spectrum, with other units more similar to hydrocarbon ''tholin'', but the results were highly sensitive to the assumed atmospheric properties. Soderblom et al (2009Soderblom et al ( , 2010 used a discrete ordinates model including collision induced broadening of gaseous absorption bands, and scattering by tholin aggregates representing Titan's aerosols, but were unable to derive absolute surface albedos with any certainty. Griffith et al (2012) applied a radiative transfer model based on the doubling and adding method, with constraints on gas and aerosol opacities in the wavelength range 0.85-1.6 lm derived from the Huygens probe's near-IR spectrometer.…”

Section: Introductionmentioning

confidence: 99%

Titan’s surface composition and atmospheric transmission with solar occultation measurements by Cassini VIMS

Hayne

McCord

Sotin

2014

Icarus

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“…Prior searches for such eruptions have been inconclusive as a result of resolution constraints (e.g., at 300 m or coarser, flow features from surface processes are difficult to distinguish from those produced by eruption of internally derived material; [106]) and the lack of an empirical prototype on which to premise the search (e.g., we do not know what a cryoflow should look like). However, paired observations, including 5-μm anomalies from VIMS, suggest that some of the flow-like materials may be recent and unique [6,137]. We would observe and interpret flow-like features at much higher spatial scale with AVIATR on Titan in the context of several leading hypotheses: cryovolcanic eruption, deposition, or dissolution.…”

Section: Task 14b Infer Geologic and Climatic History From Layering mentioning

confidence: 75%

“…Their spectra show them to be nearly free of water ice, thus making them relatively bright at 5-microns as compared to the rest of Titan [5]. The strong spectral contrast for Tui and Hotei along with their lobate shapes as viewed at near-infrared and RADAR wavelengths originally suggested that they may be cryovolcanic features [6,137,161]. While terrestrial volcanoes effuse liquid rock, since Earth's crust is made of rock, a volcano on Titan would exude Titan's crustal material in liquid form-hence the term cryovolcano.…”

Section: Huygensmentioning

confidence: 99%

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AVIATR—Aerial Vehicle for In-situ and Airborne Titan Reconnaissance

et al. 2011

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We describe a mission concept for a stand-alone Titan airplane mission: Aerial Vehicle for In-situ and Airborne Titan Reconnaissance (AVI-ATR). With independent delivery and direct-to-Earth communications, AVI-ATR could contribute to Titan science either alone or as part of a sustained Titan Exploration Program. As a focused mission, AVIATR as we have envisioned it would concentrate on the science that an airplane can do best: exploration of Titan's global diversity. We focus on surface geology/hydrology and lower-atmospheric structure and dynamics. With a carefully chosen set of seven instruments-2 near-IR cameras, 1 near-IR spectrometer, a RADAR altimeter, an atmospheric structure suite, a haze sensor, and a raindrop detector-AVIATR could accomplish a significant subset of the scientific objectives of the aerial element of flagship studies. The AVIATR spacecraft stack is composed of a Space Vehicle (SV) for cruise, an Entry Vehicle (EV) for entry and descent, and the Air Vehicle (AV) to fly in Titan's atmosphere. Using an Earth-Jupiter gravity assist trajectory delivers the spacecraft to Titan in 7.5 years, after which the AVIATR AV would operate for a 1-Earthyear nominal mission. We propose a novel 'gravity battery' climb-then-glide strategy to store energy for optimal use during telecommunications sessions. We would optimize our science by using the flexibility of the airplane platform, generating context data and stereo pairs by flying and banking the AV instead

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The geology of Hotei Regio, Titan: Correlation of Cassini VIMS and RADAR

Cited by 64 publications

References 47 publications

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

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

Titan’s surface composition and atmospheric transmission with solar occultation measurements by Cassini VIMS

AVIATR—Aerial Vehicle for In-situ and Airborne Titan Reconnaissance

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