Io’s Thermal Emission and Heat Flow

Kleer, K. de; Rathbun, J. A.

doi:10.1007/978-3-031-25670-7_6

Cited by 4 publications

(3 citation statements)

References 123 publications

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“…That the new deposit was apparently longer lasting than the 1997 deposit might be the result of less volcanic activity at Pele at present than during the Galileo era. The drop in activity manifested as a ∼75% drop in total thermal emission after the Galileo mission from 280 GW (Davies et al., 2001) to 60 GW (Davies et al., 2023; de Kleer & Rathbun, 2023; de Pater et al., 2016; Rathbun et al., 2014). A lower volumetric lava effusion rate might also suggest a similar decrease in gas emission volume (Davies, 2007).…”

Section: Discussionmentioning

confidence: 99%

“…Close to the center of the plume deposit, around the lava lake, darker material is deposited, likely clasts of silicate lava caught in the gas stream which detrain from the gas flow as the gases expand. The Pele lava lake at the center of the plume deposit is a long‐lived thermal source, although it has diminished in strength over the past decade (Davies et al., 2001; de Kleer & Rathbun, 2023; de Pater et al., 2016). Whether the amount of material being ejected has also diminished in strength has been an unanswered question as the last time this area of Io was imaged at visible wavelengths was in 2007 by New Horizons (Spencer et al., 2007) (see also NASA Photojournal image PIA09355).…”

Section: Introductionmentioning

confidence: 99%

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Observation of Io's Resurfacing via Plume Deposition Using Ground‐Based Adaptive Optics at Visible Wavelengths With LBT SHARK‐VIS

Conrad,

Pedichini,

Li Causi

et al. 2024

Geophysical Research Letters

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Since volcanic activity was first discovered on Io from Voyager images in 1979, changes on Io's surface have been monitored from both spacecraft and ground‐based telescopes. Here, we present the highest spatial resolution images of Io ever obtained from a ground‐based telescope. These images, acquired by the SHARK‐VIS instrument on the Large Binocular Telescope, show evidence of a major resurfacing event on Io's trailing hemisphere. When compared to the most recent spacecraft images, the SHARK‐VIS images show that a plume deposit from a powerful eruption at Pillan Patera has covered part of the long‐lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth‐based telescopes. The SHARK‐VIS instrument ushers in a new era of high resolution imaging of Io's surface using adaptive optics at visible wavelengths.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Observation of Io's Resurfacing via Plume Deposition Using Ground‐Based Adaptive Optics at Visible Wavelengths With LBT SHARK‐VIS

Conrad,

Pedichini,

Li Causi

et al. 2024

Geophysical Research Letters

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“…The increase and subsequent decrease typically happen over a period of order 1–2 months each, separated by a ∼3‐month period of high intensity (∼120 GW/ μ m/sr at 3.78 μm) (de Kleer & de Pater, 2017; de Pater et al., 2017; Howell et al., 2001). The most up‐to‐date Loki Patera graph of intensity versus time (de Kleer & Rathbun, 2023) shows that the volcano's last brightening event stretched over April–September 2021. Based on the 440–540 day period, the next brightening event would have been expected to start in August–October 2022.…”

Section: Discussionmentioning

confidence: 99%

An Energetic Eruption With Associated SO 1.707 Micron Emissions at Io's Kanehekili Fluctus and a Brightening Event at Loki Patera Observed by JWST

et al. 2023

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We observed Io with the James Webb Space Telescope (JWST) while the satellite was in eclipse, and detected thermal emission from several volcanoes. The data were taken as part of our JWST‐ERS program #1373 on 15 November 2022. Kanehekili Fluctus was exceptionally bright, and Loki Patera had most likely entered a new brightening phase. Spectra were taken with NIRSpec/IFU at a resolving power R ≈ 2,700 between 1.65 and 5.3 µm. The spectra were matched by a combination of blackbody curves that showed that the highest temperature, ∼1,200 K, for Kanehekili Fluctus originated from an area ∼0.25 km2 in size, and for Loki Patera this high temperature was confined to an area of ∼0.06 km2. Lower temperatures, down to 300 K, cover areas of ∼2,000 km2 for Kanehekili Fluctus, and ∼5,000 km2 for Loki Patera. We further detected the a1Δ ⇒ X3Σ− 1.707 µm rovibronic forbidden SO emission band complex over the southern hemisphere, which peaked at the location of Kanehekili Fluctus. This is the first time this emission has been seen above an active volcano, and suggests that the origin of such emissions is ejection of SO molecules directly from the vent in an excited state, after having been equilibrated at temperatures of ∼1,500 K below the surface, as was previously hypothesized.

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JIRAM Observations of Volcanic Flux on Io: Distribution and Comparison to Tidal Heat Flow Models

Pettine,

Imbeah,

Rathbun

et al. 2024

Geophysical Research Letters

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Juno has allowed clear, high‐resolution imaging of Io's polar volcanoes using the Jovian Infrared Auroral Mapper (JIRAM) instrument. We have used data from JIRAM's M‐band (4.78 μm) imager from 11 Juno orbits to construct a global map of volcanic flux. This map provides short‐term insight into the spatial distribution of volcanoes and the ways in which high‐ and low‐latitude volcanoes differ. Using spherical harmonic analysis, we quantitatively compare our volcanic flux map to the surface heat flow distribution expected from models of Io's tidal heat deposition (summarized in de Kleer, Park, et al. (2019, https://doi.org/10.26206/d4wc‐6v82). Our observations confirm previously detected systems of bright volcanoes at high latitudes. Our study finds that both poles are comparably active and that the observed flux distribution is inconsistent with an asthenospheric heating model, although the south pole is viewed too infrequently to establish reliable trends.

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Io’s Thermal Emission and Heat Flow

Cited by 4 publications

References 123 publications

Observation of Io's Resurfacing via Plume Deposition Using Ground‐Based Adaptive Optics at Visible Wavelengths With LBT SHARK‐VIS

Observation of Io's Resurfacing via Plume Deposition Using Ground‐Based Adaptive Optics at Visible Wavelengths With LBT SHARK‐VIS

An Energetic Eruption With Associated SO 1.707 Micron Emissions at Io's Kanehekili Fluctus and a Brightening Event at Loki Patera Observed by JWST

JIRAM Observations of Volcanic Flux on Io: Distribution and Comparison to Tidal Heat Flow Models

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