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Volumn 307, Issue 5713, 2005, Pages 1226-1236

Cassini Imaging Science: Initial results on Saturn's rings and small satellites

(35)  Porco, C C a   Baker, E a   Barbara, J b   Beurle, K c   Brahic, A d   Burns, J A e   Charnoz, S d   Cooper, N c   Dawson, D D f   Del Genio, A D b   Denk, T g   Dones, L h   Dyudina, U i   Evans, M W c   Giese, B j   Grazier, K k   Helfenstein, P e   Ingersoll, A P i   Jacobson, R A k   Johnson, T V k   more..


Author keywords

[No Author keywords available]

Indexed keywords

IMAGE RECONSTRUCTION; MOON; ORBITS; SATELLITES; SPACECRAFT; WAVES;

EID: 20044369347     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.1108056     Document Type: Article
Times cited : (193)

References (77)
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    • o is the value of I/F at some fiducial wavelength. Ground-based observations have shown that the main rings are "red" in the spectral range from 300 to ∼600 nm (i.e., I/F increases with wavelength, λ), whereas I/F is roughly constant from 600 to 1000 nm (71, 72). HST observations showed that the rings' spectral slope increases with phase angle over the range 0° to 6° visible from Earth. This reddening is thought to result from multiple scattering within the surfaces of ring particles (74). Our results show that little, if any, additional "phase reddening" occurs at phase angles between 6° and 66°. Color variations in Saturn's rings on a variety of spatial scales have been seen by Voyager and HST (16, 73, 74).
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    • The interpretation of dark-side images can be ambiguous: Empty space, as well as high-optical depth regions, can appear; intermediate-optical depth regions appear bright.
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    • 5, e, and i are the mass, orbital eccentricity, and inclination to Saturn's equator of the satellite, respectively. For a given moon, the strongest density waves have p = n = 0, so that these waves are of the form m:(m - 1). Waves driven by interior moons on exterior rings, like the Uranian ε ring, would have (m - 1):m for first-order waves, and (m - 2):m for second-order waves. The waves we describe in detail are Atlas and Pan waves with m = 5 and 7, respectively.
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    • note
    • We acknowledge the many individuals across the imaging team who have assisted in the design of imaging sequences and camera commands and in other vital operational and image-processing tasks, in particular E, Birath, J. Riley, B. Knowles, C. Clark, M. Belanger, and D. Wilson. M. Hedman is acknowledged for fruitful discussions. This work has been funded by NASA/JPL, the UK Partide Physics and Astronomy Research Council, the German Aerospace Center (DLR), and Université Paris VII Denis Diderot, Commissariat à l'Energie Atomique, Astrophysique Interactions Multiéchelles, France.


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.