A simple quantitative model of plasma flows and currents in Saturn's polar ionosphere

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Modeling the size and shape of Saturn's magnetopause with variable dynamic pressure (2006, background): “Also one should expect a dawn-dusk asymmetry due to flow asymmetries in the magnetosphere [Cowley et al., 2004].”
Recurrent energization of plasma in the midnight-to-dawn quadrant of Saturn's magnetosphere, and its relationship to auroral UV and radio emissions (2009, background): “This post-noon feature rotates considerably more slowly than the auroral feature associated with the ENA enhancement, and is likely driven by flow shear near or at the magnetopause as suggested for much of Saturn’s auroral emission by Cowley et al. (2004). The auroral emission associated with the EN”
Energetic particle injections in Saturn's magnetosphere (2005, methodology): “A parametric equation, inspired by Cowley et al. [2004], is used for W0:”
Reconnection in a rotation-dominated magnetosphere and its relation to Saturn's auroral dynamics (2005, background): “…by the Hubble Space Telescope (HST) over past years have indeed shown a highly variable auroral morphology [Gérard et al., 1995, 2004; Trauger et al., 1998; Cowley et al., 2004a], but in the absence of upstream data it has not been possible to relate these to concurrent interplanetary conditions.”