Viscosity in a dense planetary ring with self-gravitating particles

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Accretion of Saturn's mid-sized moons during the viscous spreading of young massive rings: Solving the paradox of silicate-poor rings versus silicate-rich moons (2011, methodology): “S is the disk’s surface and k is a numerical factor coming from the viscosity model (so that the viscosity is given by v kr2 where r is the disk’s surface density, see Daisaka et al., 2001), k 8 10 8 m6 kg2 s 1 here (see supplementary information#4 in Charnoz et al. (2010)).”
Cassini Imaging Science: Instrument Characteristics And Anticipated Scientific Investigations At Saturn (2004, background): “Further modeling of the asymmetry should provide an excellent probe of the properties of the rings, such as their viscosity (Daisaka et al., 2001).”
REBOUND: An open-source multi-purpose N-body code for collisional dynamics (2011, methodology): “The separate parts of the viscosity are calculated directly as defined by Daisaka et al. (2001) for various r h and plotted in dimensionless units in Fig.”