Laboratory Infrared Spectra (2.3-23 μm) of SO2 Phases: Applications to Io Surface Analysis

Nash, Douglas B.; Betts, Bruce

doi:10.1006/icar.1995.1165

Cited by 34 publications

(27 citation statements)

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“…The reflectance part of the spectrum contains numerous absorption bands of solid SO 2 that were assigned by Carlson et al (1997) using the work of Schmitt et al (1994) and Nash and Betts (1995). Other more modest signatures are also found, notably a broad and shallow absorption in the 1.0-to 1.3-µm region and a weak band at 3.15 µm.…”

Section: Methods and Assumptionsmentioning

confidence: 94%

Mapping SO2 Frost on Io by the Modeling of NIMS Hyperspectral Images

Douté

Schmitt

Lopes-Gautier

et al. 2001

Icarus

115

112

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Section: Methods and Assumptionsmentioning

confidence: 94%

Mapping SO2 Frost on Io by the Modeling of NIMS Hyperspectral Images

Douté

Schmitt

Lopes-Gautier

et al. 2001

Icarus

115

112

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“…Absorption positions and shapes of known and possible species are shown, including polymeric sulfur (S μ ) and polysulfur oxide (PSO) (Baklouti et al 2008). Adapted from Carlson et al (2007) Most of the absorption features characterizing Io's spectrum can be attributed to SO 2 frost (Fanale et al 1979;Hapke 1979;Smythe et al 1979;Schmitt et al 1994;Nash and Betts 1995;Carlson et al 1997) (Fig. 4).…”

Section: Iomentioning

confidence: 95%

“…4). Nash and Betts (1995) proposed Na 2 S to be responsible for the spectral feature reaching from 0.55 to 0.7 μm. Na, K, and Cl, as well as sulfur and oxygen compounds are seen escaping from Io and populating the neutral and plasma torus (McGrath et al 2004).…”

Section: Iomentioning

confidence: 99%

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 surface hemispherical emittances of SO 2 (frost) and S n (a likely non-frost component, see e.g. Geissler et al, 1999) are taken from Nash (1986) and Nash and Betts (1995), who obtained laboratory mid-infrared spectra of these materials. The reported value for the hemispherical emittance at 530.4 cm À1 is unity for SO 2 frost and 0.8 for solid sulfur.…”

Section: Longitude [Deg]mentioning

confidence: 99%