The Plumes and Atmosphere of Io

Pater, Imke de; Goldstein, David; Lellouch, E.

doi:10.1007/978-3-031-25670-7_8

Cited by 3 publications

(2 citation statements)

References 116 publications

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“…The sulfur cycle on Io is complex: sulfur moves between different reservoirs by way of multiple processes, several of which involve the atmosphere (e.g., de Pater et al., 2021, 2023; Figure 1), and most of these processes are at least potentially capable of fractionating sulfur isotopes. Based on this conceptual model, we build a numerical isotope‐enabled box model to track the four stable isotopes of sulfur over time (Figure 2; Hughes, 2024).…”

Section: Modelmentioning

confidence: 99%

Using Io's Sulfur Isotope Cycle to Understand the History of Tidal Heating

Hughes,

de Kleer,

Eiler

et al. 2024

JGR Planets

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Stable isotope fractionation of sulfur offers a window into Io's tidal heating history, which is difficult to constrain because Io's dynamic atmosphere and high resurfacing rates leave it with a young surface. We constructed a numerical model to describe the fluxes in Io's sulfur cycle using literature constraints on rates and isotopic fractionations of relevant processes. Combining our numerical model with measurements of the 34S/32S ratio in Io's atmosphere, we constrain the rates for the processes that move sulfur between reservoirs and model the evolution of sulfur isotopes over time. Gravitational stratification of SO2 in the upper atmosphere, leading to a decrease in 34S/32S with increasing altitude, is the main cause of sulfur isotopic fractionation associated with loss to space. Efficient recycling of the atmospheric escape residue into the interior is required to explain the 34S/32S enrichment magnitude measured in the modern atmosphere. We hypothesize this recycling occurs by SO2 surface frost burial and SO2 reaction with crustal rocks, which founder into the mantle and/or mix with mantle‐derived magmas as they ascend. Therefore, we predict that magmatic SO2 plumes vented from the mantle to the atmosphere will have lower 34S/32S than the ambient atmosphere, yet are still significantly enriched compared to solar‐system average sulfur. Observations of atmospheric variations in 34S/32S with time and/or location could reveal the average mantle melting rate and hence whether the current tidal heating rate is anomalous compared to Io's long‐term average. Our modeling suggests that tides have heated Io for >1.6 Gyr if Io today is representative of past Io.

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Section: Modelmentioning

confidence: 99%

Using Io's Sulfur Isotope Cycle to Understand the History of Tidal Heating

Hughes,

de Kleer,

Eiler

et al. 2024

JGR Planets

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“…Io, the innermost of Jupiter's four Galilean satellites, possesses an SO 2 ‐dominated atmosphere that is composed of sulfides, oxides, and a small amount of alkali and chlorine elements (e.g., Brown et al., 1974; Feaga et al., 2004; Feldman et al., 2000; Giono & Roth, 2021; Küppers & Schneider, 2000; Lellouch, 1996; Moullet et al., 2008; Pearl et al., 1979; Trafton, 1975). The primary source that drives Io's atmosphere is thought to be frost sublimation, with active volcanism also substantially contributing (de Pater et al., 2023, and references therein). Due to the intensive feedback interaction with Jovian magnetospheric plasma, atmospheric sputtering on Io is able to induce a massive atmospheric loss (Crary & Bagenal, 1997; Hess et al., 2007; Kabin et al., 2001).…”

Section: Introductionmentioning

confidence: 99%

A One‐Dimensional Model of Atmospheric Sputtering at Io Driven by S⁺⁺ and O⁺

Huang,

Gu,

et al. 2024

JGR Planets

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Io, the closest of Jupiter's four Galilean moons, suffers from intense ion bombardment from Jupiter's magnetosphere. The constant atmospheric erosion by energetic ion precipitation, referred to atmospheric sputtering, serves as an important mechanism of Io's atmospheric escape. This study is devoted to a state‐of‐the‐art study of atmospheric sputtering at Io, with the aid of constantly accumulated understandings of Io's space environment and atmospheric photochemistry, as well as the updated laboratory measurements. A Monte Carlo model is constructed to track the energy degradation of incident S++ and O+ and atmospheric recoils from which the sputtering yields of different atmospheric species are determined. Our calculations suggest a total escape rate of 3 × 1029 atom s−1 on Io, and SO2 is the dominant sputtered species. Further investigations reveal that S++ is the most efficient species for atmospheric sputtering on Io, and sputtering yields increase substantially with increasing incident ion mass, energy, and incidence angle. The model sensitivity to different influence factors is also discussed, including scattering angle distribution, atmospheric column density, proton precipitation, inelastic process, and surface sputtering, of which the former two dominate.

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Io’s SO₂ and NaCl Wind Fields from ALMA

Thelen,

de Kleer,

Cordiner

et al. 2024

ApJL

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We present spatially resolved measurements of SO2 and NaCl winds on Io at several unique points in its orbit: before and after eclipse and at maximum eastern and western elongation. The derived wind fields represent a unique case of meteorology in a rarified, volcanic atmosphere. Through the use of Doppler shift measurements in emission spectra obtained with the Atacama Large Millimeter/submillimeter Array between ~346 and 430 GHz (~0.70–0.87 mm), line-of-sight winds up to ~−100 m s−1 in the approaching direction and >250 m s−1 in the receding direction were derived for SO2 at altitudes of ~10–50 km, while NaCl winds consistently reached ~∣150–200∣ m s−1 in localized regions up to ~30 km above the surface. The wind distributions measured at maximum east and west Jovian elongations and on the sub-Jovian hemisphere pre- and posteclipse were found to be significantly different and complex, corroborating the results of simulations that include surface temperature and frost distribution, volcanic activity, and interactions with the Jovian magnetosphere. Further, the wind speeds of SO2 and NaCl are often inconsistent in direction and magnitude, indicating that the processes that drive the winds for the two molecular species are different and potentially uncoupled; while the SO2 wind field can be explained through a combination of sublimation-driven winds, plasma torus interactions, and plume activity, the NaCl winds appear to be primarily driven by the plasma torus.

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The Plumes and Atmosphere of Io

Cited by 3 publications

References 116 publications

Using Io's Sulfur Isotope Cycle to Understand the History of Tidal Heating

Using Io's Sulfur Isotope Cycle to Understand the History of Tidal Heating

A One‐Dimensional Model of Atmospheric Sputtering at Io Driven by S⁺⁺ and O⁺

Io’s SO₂ and NaCl Wind Fields from ALMA

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The Plumes and Atmosphere of Io

Cited by 3 publications

References 116 publications

Using Io's Sulfur Isotope Cycle to Understand the History of Tidal Heating

Using Io's Sulfur Isotope Cycle to Understand the History of Tidal Heating

A One‐Dimensional Model of Atmospheric Sputtering at Io Driven by S++ and O+

Io’s SO2 and NaCl Wind Fields from ALMA

Contact Info

Product

Resources

About

A One‐Dimensional Model of Atmospheric Sputtering at Io Driven by S⁺⁺ and O⁺

Io’s SO₂ and NaCl Wind Fields from ALMA