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Volumn 318, Issue 5856, 2007, Pages 1602-1607

Saturn's small inner satellites: Clues to their origins

Author keywords

[No Author keywords available]

Indexed keywords

MOON; NUMERICAL MODEL; SATURN; TOPOGRAPHY;

EID: 36849010220     PISSN: 00368075     EISSN: 10959203     Source Type: Journal    
DOI: 10.1126/science.1143977     Document Type: Article
Times cited : (140)

References (33)
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    • Masses are unavailable for the Trojans of Tethys (Calypso and Telesto) and Dione Helene and Polydeuces, as well as the tiny satellite-region moons Methone, Anthe, Pallene, and Polydeuces, because none of these is massive enough to measurably perturb any nearby or resonant moons
    • Masses are unavailable for the Trojans of Tethys (Calypso and Telesto) and Dione (Helene and Polydeuces), as well as the tiny satellite-region moons Methone, Anthe, Pallene, and Polydeuces, because none of these is massive enough to measurably perturb any nearby or resonant moons.
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    • It is reasonable to question the assumption that the moonlets are point masses in calculating the Roche lobe dimensions (shape and critical density) because they are clearly extended bodies. However, no self-gravitating extended body with a homogeneous interior and the low densities found for the moons in this study is even stable in the ring region, and bodies with dense cores and under-dense mantles differ in their dimensions from those of a point-mass Roche lobe by at most ∼5
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    • We thank the staff members of CICLOPS and B. Carcich (Cornell University) for technical support, and L. Dones for fruitful discussions. Supported by NASA Planetary Geology and Geophysics grant NAG5-4451 and the Cassini Project
    • We thank the staff members of CICLOPS and B. Carcich (Cornell University) for technical support, and L. Dones for fruitful discussions. Supported by NASA Planetary Geology and Geophysics grant NAG5-4451 and the Cassini Project.


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.