| People | Locations | Statistics |
|---|---|---|
| Naji, M. |
| |
| Motta, Antonella |
| |
| Aletan, Dirar |
| |
| Mohamed, Tarek |
| |
| Ertürk, Emre |
| |
| Taccardi, Nicola |
| |
| Kononenko, Denys |
| |
| Petrov, R. H. | Madrid |
|
| Alshaaer, Mazen | Brussels |
|
| Bih, L. |
| |
| Casati, R. |
| |
| Muller, Hermance |
| |
| Kočí, Jan | Prague |
|
| Šuljagić, Marija |
| |
| Kalteremidou, Kalliopi-Artemi | Brussels |
|
| Azam, Siraj |
| |
| Ospanova, Alyiya |
| |
| Blanpain, Bart |
| |
| Ali, M. A. |
| |
| Popa, V. |
| |
| Rančić, M. |
| |
| Ollier, Nadège |
| |
| Azevedo, Nuno Monteiro |
| |
| Landes, Michael |
| |
| Rignanese, Gian-Marco |
|
Brown, R. H.
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (6/6 displayed)
- 2017From the Icy Satellites to Small Moons and Rings: Spectral Indicators by Cassini-VIMS Unveil Compositional Trends in the Saturnian System
- 2013Surface Composition of the Non-Ice Component on Icy Satellites and Ring Particles in the Saturn System
- 2011The Composition of Saturn's Rings and Satellites from Cassini VIMS and UVIS
- 2010Spectrophotometric Modeling of Enceladus Surface Properties and Composition from Vims Data
- 2008The Composition of Saturn's Rings
- 2007Saturn's Rings Observed with Cassini-VIMS
Places of action
| Organizations | Location | People |
|---|
document
The Composition of Saturn's Rings and Satellites from Cassini VIMS and UVIS
Abstract
Spectra of the rings and icy satellites of Saturn from Cassini UVIS and VIMS, covering from ~0.1 to 5.1 microns show both expected and unusual properties. The spectra of all these objects are dominated by absorption and scattering by water-ice grains, variable amounts of a non-ice material that is strongly absorbing with a stronger UV absorption, small and variable amounts of CO2 and trace amounts of CH compounds, trapped H2, and possible trace NH compounds. The dark material seems to contain the trapped H2, CO2 and NH compounds. Classical interpretations of the UV absorber and dark material are varying amounts of tholins and carbon. A newer interpretation is that the main spectral components are ice + nano-grains of metallic iron, and nano-hematite. Iron is an efficient H2 trap. Iron has the highest absorption coefficient we have found, approaching one million per cm at 0.25 microns. Nano-sized grains create both Rayleigh absorption and Rayleigh scattering producing the variable spectral signatures seen in the Saturn system. The large spectral range of combined UVIS + VIMS spectra provide strong constraints on composition and grain size distribution. Spectra of the rings and all icy satellites indicate a large range of ice grain sizes, from tens of microns to sub-micron. Sub-micron ice grains create unusual spectral properties, including decreased reflectance near 5-microns, decreased 3.1-micron Fresnel peak, decreased 2.6-micron reflectance, asymmetric to longer wavelength 2-micron absorption, reduced 1.5/2-micron ice band depth ratio, and enhanced reflectance at shorter wavelengths, all of which are seen in the spectra of the rings and satellites. In the blue/UV, spectra of the rings and satellites depart from that of ice because of the UV absorber. Some spectra of Saturn's rings are very similar to spectra of some locations on icy satellites, indicating common compounds are spectrally active from the rings to Iapetus. Sub-micron ice grains create Rayleigh scattering into the UV which competes with the UV absorber to create the various spectral shapes seen in the Saturn system. <P />...