Regular ArticleNear-Infrared Absolute Photometric Imaging of the Uranian System☆
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Cited by (28)
Modeling the uranian rings at 2.2μm: Comparison with Keck AO data from July 2004
2010, IcarusCitation Excerpt :The optical depths are fairly well established (see Table 4), but there is a variance in some rings and the amount of dust may vary over time, which would significantly change I/F (see Fig. 3b). The single-scattering albedo could be as high as ϖ0 = 0.08 (e.g. Karkoschka, 2001b), but most likely below ϖ0 < 0.10 and may be as low as ϖ0 ∼ 0.3–0.4 for the macroscopic rings (e.g. Baines et al., 1998). The will reduce the amount of multiple scattering which would be important even in the dust rings at low B if ϖ were larger.
New cloud activity on Uranus in 2004: First detection of a southern feature at 2.2 μm
2005, IcarusCitation Excerpt :The serendipitous discovery of discrete clouds on Uranus in the satellite-search images revitalized interest in the planet's atmosphere (Hammel, 1997), which had been muted since the Voyager Uranus encounter showing little atmospheric activity (Smith et al., 1986). Ground-based images in 1995 from the NASA Infrared Telescope Facility (IRTF) had resolved the disk, but discrete features were not detected (Baines et al., 1998). Beginning in 1997, however, HST observed Uranus with both the Near-Infrared Camera and Multi-Object Spectrograph (NICMOS) and the Wide Field Planetary Camera 2 (WFPC2), revealing many atmospheric features in both hemispheres (Karkoschka, 1998, 2001; Hammel et al., 2001).
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J. T. BergstralhE. D. MinerM. S. Matthews