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One of the biggest successes of the Cassini mission is the detection of smallmoons (moonlets) embedded in Saturn's rings which cause S-shaped densitystructures in their close vicinity, called propellers (Spahn and Sremcevic2000; Tiscareno et al. 2006; Sremcevic et al. 2007). Here, we presentisothermal hydrodynamic simulations of moonlet-induced propellers in Saturn's Aring which denote a further development of the original model (Spahn andSremcevic 2000). We find excellent agreement between these new hydrodynamic andcorresponding N-body simulations. Furthermore, the hydrodynamic simulationsconfirm the predicted scaling laws (Spahn and Sremcevic 2000) and theanalytical solution for the density in the propeller gaps (Sremcevic et al.2002). Finally, this mean field approach allows us to simulate the pattern ofthe giant propeller Bleriot, which is too large to be modeled by direct N-bodysimulations. Our results are compared to two stellar occultation observationsby the Cassini Ultraviolet Imaging Spectrometer (UVIS), that intersect thepropeller Bleriot. Best fits to the UVIS optical depth profiles are achievedfor a Hill radius of 590 m, which implies a moonlet diameter of about 860 m.Furthermore, the model favours a kinematic shear viscosity of the surroundingring material of $\nu_0 = 340$ cm^2/s, a dispersion velocity in the range of0.3 cm/s $< c_0 <$ 1.5 cm/s, and a fairly high bulk viscosity $7 < \xi_0/\nu_0< 17$. These large transport values might be overestimated by our isothermalring model and should be reviewed by an extended model including thermalfluctuations.

Hydrodynamic simulations of moonlet induced propellers in Saturn's rings: Application to Bleriot