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Cassini SAR, radiometry, scatterometry and altimetry observations of Titan’s dune fields
► Dune fields is the largest known organic reservoir on Titan. ► To first order, dune fields are less emissive and brighter as one goes north (up to a latitude of ∼11°). ► This is primarily due to an increasing fraction of bright interdunes towards high latitudes. ► This could indicate an asymmetry...
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Published in: | Icarus (New York, N.Y. 1962) N.Y. 1962), 2011-06, Vol.213 (2), p.608-624 |
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Main Authors: | , , , , , , , , , , , , , , |
Format: | Article |
Language: | English |
Subjects: | |
Citations: | Items that this one cites Items that cite this one |
Online Access: | Get full text |
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Summary: | ► Dune fields is the largest known organic reservoir on Titan. ► To first order, dune fields are less emissive and brighter as one goes north (up to a latitude of ∼11°). ► This is primarily due to an increasing fraction of bright interdunes towards high latitudes. ► This could indicate an asymmetry in the available sediment supply or ground humidity.
Large expanses of linear dunes cover Titan’s equatorial regions. As the Cassini mission continues, more dune fields are becoming unveiled and examined by the microwave radar in all its modes of operation (SAR, radiometry, scatterometry, altimetry) and with an increasing variety of observational geometries. In this paper, we report on Cassini’s radar instrument observations of the dune fields mapped through May 2009 and present our key findings in terms of Titan’s geology and climate. We estimate that dune fields cover ∼12.5% of Titan’s surface, which corresponds to an area of ∼10
million
km
2, roughly the area of the United States. If dune sand-sized particles are mainly composed of solid organics as suggested by VIMS observations (Cassini Visual and Infrared Mapping Spectrometer) and atmospheric modeling and supported by radiometry data, dune fields are the largest known organic reservoir on Titan. Dune regions are, with the exception of the polar lakes and seas, the least reflective and most emissive features on this moon. Interestingly, we also find a latitudinal dependence in the dune field microwave properties: up to a latitude of ∼11°, dune fields tend to become less emissive and brighter as one moves northward. Above ∼11° this trend is reversed. The microwave signatures of the dune regions are thought to be primarily controlled by the interdune proportion (relative to that of the dune), roughness and degree of sand cover. In agreement with radiometry and scatterometry observations, SAR images suggest that the fraction of interdunes increases northward up to a latitude of ∼14°. In general, scattering from the subsurface (volume scattering and surface scattering from buried interfaces) makes interdunal regions brighter than the dunes. The observed latitudinal trend may therefore also be partially caused by a gradual thinning of the interdunal sand cover or surrounding sand sheets to the north, thus allowing wave penetration in the underlying substrate. Altimetry measurements over dunes have highlighted a region located in the Fensal dune field (∼5° latitude) where the icy bedrock of Titan is likely expose |
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ISSN: | 0019-1035 1090-2643 |
DOI: | 10.1016/j.icarus.2011.03.026 |