Compositional analysis of Hyperion with the Cassini Visual and Infrared Mapping Spectrometer

Dalton, J. B.; Cruikshank, D. P.; Clark, R. N.

doi:10.1016/j.icarus.2012.05.003

Cited by 12 publications

(8 citation statements)

References 43 publications

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“…Thomas et al (2007a) use the observation of sub-km-sized craters on the floors of larger craters to argue that there has been <20 m of eroded material transported out onto these floors, and hence CO 2 sublimation, if acting, may be limited. Brad Dalton et al (2012) report pure H 2 O ice, probably as frosts, preferentially located atop topographic crests (crater rims), which is consistent with local volatile redistribution and cold trapping.…”

Section: Background and Initial Working Hypothesesmentioning

confidence: 52%

“…This blanketing is primarily but not exclusively concentrated in basin interiors, but it appears to be a thin, recent mantle whose origin may be unrelated to the mass wasting landforms investigated here. However, the possibility that it is a local detritus created by the loss of cementing volatiles upslope cannot be ruled out (Brad Dalton et al, 2012).…”

Section: Surface Morphologymentioning

confidence: 99%

“…We assume that the bedrock of Hyperion consists of a mixture of frozen volatiles (H 2 O, CO 2 and possibly others (Cruikshank et al, 2007;Brad Dalton et al, 2012)) mixed with non-volatile particulates (e.g. silicates and carbon).…”

Section: Bedrock Weatheringmentioning

confidence: 99%

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Sublimation-driven erosion on Hyperion: Topographic analysis and landform simulation model tests

Howard

Moore

Schenk

et al. 2012

Icarus

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Section: Background and Initial Working Hypothesesmentioning

confidence: 52%

Section: Surface Morphologymentioning

confidence: 99%

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Sublimation-driven erosion on Hyperion: Topographic analysis and landform simulation model tests

Howard

Moore

Schenk

et al. 2012

Icarus

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“…CO2 was also found in the dark terrains on Iapetus and was interpreted as a product of irradiating H2O + carbonaceous material such as hydrocarbons (Buratti et al 2005;Palmer & Brown 2011). Similar ice "contaminants" have been found on Hyperion (Tosi et al 2010;Dalton et al 2012), consistent with a common source of surface material for Saturn's three mid-sized moons orbiting beyond Titan. The later discovery of similar dark material on Dione and its spatial distribution there supported a hypothesis that this material arrived at all of these satellites from a source outside the Saturnian system (Clark et al 2008;Stephan et al 2010), while the discovery of the Phoebe ring in 2009 led to conclusions that dark particles were transported to Iapetus and Hyperion from Phoebe (Tosi et al 2010).…”

Section: Introductionmentioning

confidence: 61%

Silicates on Iapetus From Cassini’s Composite Infrared Spectrometer

Young

Wray

Clark

et al. 2015

ApJ

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We present the first spectral features obtained from Cassini's Composite Infrared Spectrometer (CIRS) for any icy moon. The spectral region covered by CIRS focal planes (FP) 3 and 4 is rich in emissivity features, but previous studies at these wavelengths have been limited by low signal-to-noise ratios (S/Ns) for individual spectra. Our approach is to average CIRS FP3 spectra to increase the S/N and use emissivity spectra to constrain the composition of the dark material on Iapetus. We find an emissivity feature at ∼855 cm −1 and a possible doublet at 660 and 690 cm −1 that do not correspond to any known instrument artifacts. We attribute the 855 cm −1 feature to fine-grained silicates, similar to those found in dust on Mars and in meteorites, which are nearly featureless at shorter wavelengths. Silicates on the dark terrains of Saturn's icy moons have been suspected for decades, but there have been no definitive detections until now. Serpentines reported in the literature at ambient temperature and pressure have features near 855 and 660 cm −1. However, peaks can shift depending on temperature and pressure, so measurements at Iapetus-like conditions are necessary for more positive feature identifications. As a first investigation, we measured muscovite at 125 K in a vacuum and found that this spectrum does match the emissivity feature near 855 cm −1 and the location of the doublet. Further measurements are needed to robustly identify a specific silicate, which would provide clues regarding the origin and implications of the dark material.

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“…Orbiting between Iapetus and Titan, Hyperion receives an optically significant coating of particles of order 5 lm in size, distributed more or less uniformly over the surface as a consequence of Hyperion's chaotic rotation. The nature of the dark material in the context of Hyperion's surface is explored in more detail by Dalton et al (2012).…”

Section: Introductionmentioning

confidence: 99%