The Spectrum of Sulfur and its Allotropes

Meyer, B.; Gouterman, Martin; Jensen, Detlef; Oommen, T. V.; Spitzer, K.; Stroyer‐Hansen, T.

doi:10.1021/ba-1972-0110.ch004

Cited by 46 publications

(31 citation statements)

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“…Otherwise, we may survey related data for small chalcogen clusters. For S, Averkiev et al [7] reports for S-loaded NaA zeolite three absorption bands at 2-3 eV, attributing to S 3 and S 4 clusters, which is consistent with results obtained by Meyer et al for red S [32].…”

Section: Discussionsupporting

confidence: 85%

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Optical properties of chalcogen-loaded zeolite (ZSM-5)

Saitoh

Tanaka

2009

Solid State Communications

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Sulfur, selenium, and tellurium were loaded into sub-mm size ZSM-5 single crystals and the optical properties have been comparatively studied. S and Te show similar features, while Se is unique. S and Te have optical absorption edges at wavelengths of ~400 nm with transmission dips at ~450 nm, while Se has the edge at ~550 nm. The three materials provide photoluminescence at visible wavelengths, with intensities of S and Te being stronger than that of Se by two orders. These optical properties imply that S and Te in the zeolite form small atomic units such as S 3 and Te 2 , while Se condenses into single-chain structures.

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Section: Discussionsupporting

confidence: 85%

“…This model is consistent with the absorption spectra. For z-S, it seems that S 2 governs the absorption edge at ~3 eV [7,32] and an absorbance peak at ~2.8 eV arises from S 3 chains. For Se, single chains can be geometrically incorporated into the ZSM-5 pores.…”

Section: Discussionmentioning

confidence: 99%

Optical properties of chalcogen-loaded zeolite (ZSM-5)

Saitoh

Tanaka

2009

Solid State Communications

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“…10. The shift is well documented in S 8 rings (Meyer et al 1972). Temperature-dependent color changes and a similar shift in the absorption edge occurs in other forms of sulfur, including some formed by quenching and contamination, although the mechanism is not well understood and might depend on the ratios of sulfur allotropes, hence, composition.…”

Section: The Composition Of Io's Surfacementioning

confidence: 81%

Volcanogenic Sulfur on Earth and Io: Composition and Spectroscopy

Kargel

Delmelle

Nash

1999

Icarus

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“…Above 368 K, an alternative form, monoclinic sulfur, becomes thermodynamically preferred (Meyer 1976). A key feature of orthorhombic sulfur's complex refractive index is the increase in k at shorter wavelengths caused by vibrational modes in the S 8 molecules, which tend to become more populated at higher temperatures, thereby shifting the increase in k to longer wavelengths (Meyer et al 1972). Increased absorption at shorter wavelengths will lead to sulfur-haze-enveloped exoplanets being yellowish to reddish in color.…”

Section: Sulfur In Giant Exoplanetsmentioning

confidence: 99%

Sulfur Hazes in Giant Exoplanet Atmospheres: Impacts on Reflected Light Spectra

Gao

Marley

Zahnle

et al. 2017

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Recent work has shown that sulfur hazes may arise in the atmospheres of some giant exoplanets, due to the photolysis of H 2 S. We investigate the impact such a haze would have on an exoplanet's geometric albedo spectrum and how it may affect the direct imaging results of the Wide Field Infrared Survey Telescope (WFIRST), a planned NASA space telescope. For temperate (250 K<T eq <700 K) Jupiter-mass planets, photochemical destruction of H 2 S results in the production of ∼1 ppmv of S 8 between 100 and 0.1 mbar, which, if cool enough, will condense to form a haze. Nominal haze masses are found to drastically alter a planet's geometric albedo spectrum: whereas a clear atmosphere is dark at wavelengths between 0.5 and 1 μm, due to molecular absorption, the addition of a sulfur haze boosts the albedo there to ∼0.7, due to scattering. Strong absorption by the haze shortward of 0.4 μm results in albedos <0.1, in contrast to the high albedos produced by Rayleigh scattering in a clear atmosphere. As a result, the color of the planet shifts from blue to orange. The existence of a sulfur haze masks the molecular signatures of methane and water, thereby complicating the characterization of atmospheric composition. Detection of such a haze by WFIRST is possible, though discriminating between a sulfur haze and any other highly reflective, high-altitude scatterer will require observations shortward of 0.4 μm, which is currently beyond WFIRST's design.

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The Spectrum of Sulfur and its Allotropes

Cited by 46 publications

References 0 publications

Optical properties of chalcogen-loaded zeolite (ZSM-5)

Optical properties of chalcogen-loaded zeolite (ZSM-5)

Volcanogenic Sulfur on Earth and Io: Composition and Spectroscopy

Sulfur Hazes in Giant Exoplanet Atmospheres: Impacts on Reflected Light Spectra

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