Io: Heat flow from dark volcanic fields

Veeder, G. J.; Davies, A. G.; Matson, D. L.; Johnson, T. V.

doi:10.1016/j.icarus.2009.06.027

Cited by 28 publications

(13 citation statements)

References 80 publications

(326 reference statements)

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“…The Marduk Fluctus volcanic complex as seen by the Galileo Solid-State Imaging experiment. The area of the young, black lava flows is ≈3,600 km 2 (Veeder et al, 2009. The reddish deposit is rich in sulfur.…”

Section: Marduk Fluctusmentioning

confidence: 98%

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Discovery of a Powerful, Transient, Explosive Thermal Event at Marduk Fluctus, Io, in Galileo NIMS Data

Davies

Veeder

et al. 2018

Geophysical Research Letters

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Analysis of Galileo Near‐Infrared Mapping Spectrometer observations of Marduk Fluctus, a volcano on the Jovian moon Io, reveals a style of volcanic activity not previously seen there—a powerful thermal event lasting only a few minutes in 1996. The thermal emission rapidly fades, suggesting extremely rapid cooling of small clasts. The duration and evolution of the explosive eruption are akin to what might be expected from a strombolian or vulcanian explosion. The presence of such events provides an additional volcanic process that can be imaged by future missions with the intent of determining lava composition from eruption temperature, an important constraint on the internal composition of Io. These data promise to be of particular use in understanding the mechanics of explosive volcanic processes on Io.

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Section: Marduk Fluctusmentioning

confidence: 98%

“…The area is marked by what are presumably older flows which have cooled to the point where sulfur and SO 2 condense on the surface, yielding higher albedos than the active flows. The area of the young, black lava flows is ≈3,600 km 2 (Veeder et al, 2009.…”

Section: Marduk Fluctusmentioning

confidence: 99%

Discovery of a Powerful, Transient, Explosive Thermal Event at Marduk Fluctus, Io, in Galileo NIMS Data

Davies

Veeder

et al. 2018

Geophysical Research Letters

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“…The lower-limit endogenic power emitted by Io was estimated to be 1.05 ± 0.12 × 10 14 W (Veeder et al, 1994). Veeder et al (2009Veeder et al ( , 2011Veeder et al ( , 2012Veeder et al ( , 2015 estimated the total thermal emission from all active and recently active volcanic centers on Io, totaling 250 discrete sources (Figure 2.3). These volcanic centers accounted for 56.2 TW, or about 54% of Io's total thermal emission (using the estimate from Veeder et al, 1994).…”

Section: Global Average Heat Flowmentioning

confidence: 99%

Does Io Have a Magma Ocean?

McEwen¹,

Kleer²,

Park³

2019

Eos

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“…Relative movement of these plates stimulates planet-wide geochemical recycling via subduction, gives rise to magmatism in addition to plume-related mantle melting, and may buffer Earth's hydrosphere and atmosphere by controlling flux of volatile elements such as H2O and CO2. In contrast, Mercury, Venus, Mars and other bodies such as the Moon and Io are 'single plate' (Johnson and Hauck II, 2016;Plesa et al, 2018;Smrekar et al, 2018;Veeder et al, 2009;Wieczorek et al, 2006) and have convective regimes in which a thick 'stagnant lid' overlies the convecting mantle, at least until the point where heat loss renders bodies geologically inactive. Plume-related upwellings within a stagnant lid regime dominate volcanic activity and interior-to-surface flux of material, and limited recycling of material back into the deep interior is only possible by delamination of the parts of the lid or localised lid melting (Elkins-Tanton et al, 2007), although limited subduction has been proposed on Venus (Schubert and Sandwell, 1995) possibly related to plume upweliing (Davaille et al, 2017).…”

Section: Introductionmentioning

confidence: 99%

Diffusion of volatiles in hot stagnant-lid regime planets

Bromiley

2020

Planetary and Space Science

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Earth is unique within our solar system in having a convective regime dominated by plate tectonic processes. More typical of rocky, 'terrestrial' planets is a "stagnant lid" regime, where the entire lithosphere is a single plate, variably punctured by plume-driven volcanic activity.As such, a signficant fraction of 'Earth-like' exoplanets might instead have stagnant lids. For hot stagnant lid planets like Venus, high temperatures towards the base of the lid mean that solid-state diffusion potentially provides a mechanism for redistributing lighter, faster-diffusing volatile elements such as H. To investigate the importance of this mechanism a 1-d model is used to constrain volatile flux from a realtively undegassed planetry interior into a hot stagnant lid. Diffusion only results in signficant flux of H through an oxidised lid; diffusion of H in reduced stagnant lids and diffusion of other volatile elements, is inconsequential. For modelled Venusian tempearture profiles H diffusion fronts progress a limited distance (10s of km) into the lid over Gyr timescales. However, for a small relative increase in lid temperature (i.e. a slightly hotter than Venus exoplanet), H diffusion into the lid becomes considerable over shorter timescales. H flux upwards into the lid eventually stagnates with decreasing temperature. However, H flux markedly reduces mantle solidus in lower portions of the lid, decreasing lid stability and promoting lid rejuvination. Given the inlfuence of H on a range of mantle properties from melt relations to rheology, future models of stagnant lid planetary evolution should assess the role of diffusion in redistributing H.

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Io: Heat flow from dark volcanic fields

Cited by 28 publications

References 80 publications

Discovery of a Powerful, Transient, Explosive Thermal Event at Marduk Fluctus, Io, in Galileo NIMS Data

Discovery of a Powerful, Transient, Explosive Thermal Event at Marduk Fluctus, Io, in Galileo NIMS Data

Does Io Have a Magma Ocean?

Diffusion of volatiles in hot stagnant-lid regime planets

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