Jupiter's dawnside outer magnetosphere can be characterized as a battleground between internally driven sunward flow and solar wind-driven tailward flow, leading to a highly variable and poorly understood region of the magnetosphere. Prior to the Pioneer spacecraft encounters, the "planetary wind" model was proposed, whereby centrifugal stresses dominate when flows exceed the local Alfvén speed (Kennel & Coroniti, 1977). A key aspect of this model is the generation of internal shocks, an abrupt breakdown in corotation, and radial outflow of plasma. The planetary wind model was not supported by Voyager observations, which instead showed persistent corotation and no internal shocks. Following the Voyager 1 flyby, an extended region along the dawn flank was characterized as a "boundary layer" or "magnetospheric wind" that was distinctly different from the equatorially confined magnetodisc (Gurnett et al., 1980;Krimigis et al., 1979). Vasyliunas (1983) developed a model for