Ozone Synthesis on the Icy Satellites

Teolis, B. D.; Loeffler, M. J.; Raut, U.; Famá, M.; Baragiola, R. A.

doi:10.1086/505743

Cited by 60 publications

(55 citation statements)

References 30 publications

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“…In fact, the production and trapping of O 2 in irradiated ice have been demonstrated in multiple experiments. 18,19,[24][25][26][27][28][29][30][31] These observations lead to the suggestion that absorption bands of condensed O 2 in the reflectance spectra of Ganymede, 32 Europa, and Callisto 33 are due to high concentrations of radiolytic oxygen in the irradiated surface ice of these satellites. 34 However, this hypothesis was called into question by Vidal et al 35 and Baragiola and Bahr, 36 who found rapid outdiffusion of O 2 from unirradiated vapor-deposited O 2 -H 2 O ice mixtures at the reported Ganymede surface temperatures ͑90-152 K 37 ͒.…”

Section: Introductionmentioning

confidence: 94%

“…Although the low-energy electron studies have not regarded trapped O 2 as a precursor to O 2 emission, this assumption is difficult to reconcile with the recent thermal desorption results for ion 23,26,31 and electron-irradiated 19,27,28 ice suggesting the production and retention of trapped O 2 up to ϳ150 K. If present, trapped oxygen will contribute to the O 2 desorption yield in both electron and ion-irradiated ice since, in both cases, sputtering will eventually erode a thickness of ice sufficient to expose and eject O 2 trapped below the surface. But how does the contribution of trapped O 2 compare with that of other precursor species?…”

Section: Introductionmentioning

confidence: 97%

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Formation, trapping, and ejection of radiolytic O2 from ion-irradiated water ice studied by sputter depth profiling

Teolis

Shi

Baragiola

2009

The Journal of Chemical Physics

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We report experimental studies of 100 keV Ar(+) ion irradiation of ice leading to the formation of molecular oxygen and its trapping and ejection from the surface, at temperatures between 80 and 150 K. The use of a mass spectrometer and a quartz-crystal microbalance and sputter depth profiling at 20 K with low energy Ar ions allowed us to obtain a consistent picture of the complex radiolytic mechanism. We show that the dependence of O(2) sputtering on ion fluence is mainly due to the buildup of trapped O(2) near the surface. A small proportion of the O(2) is ejected above 130 K immediately upon creation from a precursor such as OH or H(2)O(2). The distribution of trapped oxygen peaks at or near the surface and is shallower than the ion range. Measurements of sputtering of H(2) help to elucidate the role of this molecule in the process of O(2) formation: out-diffusion leading to oxygen enrichment near the surface. The competing phenomena of OH diffusion away from the ion track and hydrogen escape from the ice and their temperature dependence are used to explain the finding of opposite temperature dependencies of O(2) and H(2)O(2) synthesis. Based on the new data and understanding, we discuss the application of our findings to ices in the outer solar system and interstellar space.

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Section: Introductionmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 97%

Formation, trapping, and ejection of radiolytic O2 from ion-irradiated water ice studied by sputter depth profiling

Teolis

Shi

Baragiola

2009

The Journal of Chemical Physics

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“…Irradiation of oxygen-rich ice surfaces can produce ozone (Teolis et al 2006) and this species has been observed on Ganymede (Noll et al 1996a(Noll et al , 1996c. Radiolysis of water ice also produces hydrogen peroxide, first found on Europa using infrared and ultraviolet spectra (Carlson et al 1999a) and later inferred from ultraviolet measurements to exist on Ganymede and Callisto (Hendrix et al 1999;Lopes et al 2008).…”

Section: Other Speciesmentioning

confidence: 98%

Chemical Composition of Icy Satellite Surfaces

et al. 2010

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Much of our knowledge of planetary surface composition is derived from remote sensing over the ultraviolet through infrared wavelength ranges. Telescopic observations and, in the past few decades, spacecraft mission observations have led to the discovery of many surface materials, from rock-forming minerals to water ice to exotic volatiles and organic compounds. Identifying surface materials and mapping their distributions allows us to constrain interior processes such as cryovolcanism and aqueous geochemistry.The recent progress in understanding of icy satellite surface composition has been aided by the evolving capabilities of spacecraft missions, advances in detector technology, and laboratory studies of candidate surface compounds. Pioneers 10 and 11, Voyagers I and II, Galileo, Cassini and the New Horizons mission have all made significant contributions. Dalton (Space Sci. Rev., 2010, this issue) summarizes the major constituents found or inferred to exist on the surfaces of the icy satellites (cf. Table 1 from Dalton, Space Sci. Rev., 2010, this issue), and the spectral coverage and resolution of many of the spacecraft instruments that have revolutionized our understanding (cf. Table 2 from Dalton, Space Sci. Rev., A. Coustenis Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Observatoire de Paris-Meudon, 5, pl. Jules Janssen,

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“…The O 3 is likely formed in the O 2 voids described above (Johnson and Jesser 1997); however, O 3 is not observed on pure ice irradiated in vacuum except when irradiation and H 2 O vapor deposition occur simultaneously (Teolis et al 2006). The O 3 -like feature is superimposed on a very broad UV absorption shortward of 0.4 µm seen on most of the icy satellites.…”

Section: Water Ice Radiolysismentioning

confidence: 99%

Radiolysis and Photolysis of Icy Satellite Surfaces: Experiments and Theory

et al. 2010

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The transport and exchange of material between bodies in the outer solar system is often facilitated by their exposure to ionizing radiation. With this in mind we review the effects of energetic ions, electrons and UV photons on materials present in the outer solar system. We consider radiolysis, photolysis, and sputtering of low temperature solids. Radiolysis and photolysis are the chemistry that follows the bond breaking and ionization produced by incident radiation, producing, e.g., O 2 and H 2 from irradiated H 2 O ice. Sputtering is the ejection of molecules by incident radiation. Both processes are particularly effective on ices in the outer solar system. Materials reviewed include H 2 O ice, sulfur-containing compounds T. Cassidy et al. (such as SO 2 and S 8 ), carbon-containing compounds (such as CH 4 ), nitrogen-containing compounds (such as NH 3 and N 2 ), and mixtures of those compounds. We also review the effects of ionizing radiation on a mixture of N 2 and CH 4 gases, as appropriate to Titan's upper atmosphere, where radiolysis and photolysis produce complex organic compounds (tholins).

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Ozone Synthesis on the Icy Satellites

Cited by 60 publications

References 30 publications

Formation, trapping, and ejection of radiolytic O2 from ion-irradiated water ice studied by sputter depth profiling

Formation, trapping, and ejection of radiolytic O2 from ion-irradiated water ice studied by sputter depth profiling

Chemical Composition of Icy Satellite Surfaces

Radiolysis and Photolysis of Icy Satellite Surfaces: Experiments and Theory

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