Carbon Dioxide and Other Materials in the Surfaces of Iapetus and Dione

Details Carbon Dioxide and Other Materials in the Surfaces of Iapetus and Dione Carbon Dioxide and Other Materials in the Surfaces of Iapetus and Dione

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.6105h&link_type=abstract

American Astronomical Society, DPS meeting #40, #61.05; Bulletin of the American Astronomical Society, Vol. 40, p.510

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Scientific paper

The two most abundant trace materials on the icy Saturnian satellites are CO2 [1] and an as yet unidentified material responsible for the 2.42-µm band [2]. Other than water ice and the dark, nonice material(s), these two substances are the only ones whose spectral features are sufficiently strong that they can be mapped. Both the CO2 and the 2.42-µm absorber are most abundant on Iapetus, Phoebe, Hyperion, and Dione [3], with the 2.42-µm band also being detected on all the satellites as well as in the F-ring [4]. The CO2 band is strongest in spectra dominated by nonice material, suggesting that the nonice material may be its host. As on the icy Galilean satellites, CO2 ice is not stable on the icy Saturnian satellites, except possibly at the poles [5]. Improvements upon the standard radiometric and wavelength calibration applied to select VIMS observations of Dione and Iapetus that have good resolution, spatial coverage, and high signal has allowed us to map the strength and shape of the CO2 and 2.42-µm bands on those satellites. The shape of the CO2 band varies between satellites [4], and varies between 4.27 and 4.28 µm on different parts of Iapetus (this work and Clark et al., pers. comm.). The spectral differences imply either a different bonding mechanism (and thus energy) and/or a different host materials on these icy satellites. On Iapetus the 2.42-µm band is present almost everywhere, with preliminary results suggesting it also is stronger in the nonice material. This work has been supported by the NASA Cassini Data Analysis Program.
References: [1] Brown et al., 2006, [2] Clark et al., Nature, 435, 66-69, 2005; [3] Filacchione et al., 2007; [4] Clark et al., Icarus, 193, 372-386, 2008; [5] Palmer, E.E. & R. Brown, Icarus, 195, 434-446, 2008.

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