There has been considerable debate regarding the nature of the solar wind interaction with the giant planet magnetospheres (Cowley et al., 2008;Masters, 2018;McComas & Bagenal, 2007). Following the New Horizons excursion down Jupiter's magnetotail, McComas and Bagenal (2008) suggested that Jupiter's interaction with the solar wind was fundamentally different from Earth due to the lack of a well-defined and tailward-extending plasma sheet. While the 10-hr rotation period of the planet was observed near the magnetopause boundary, most of the magnetotail did not exhibit a magnetic connection to the planet, with iongenic material filling much of the magnetotail cross section. Delamere and Bagenal (2010) and proposed that viscous-like stresses at the magnetopause boundary could be the dominant mechanism, facilitating the solar wind interaction. In particular, the flow shear-driven Kelvin-Helmholtz (KH) instability was suggested as a dominant mechanism to transport mass, momentum, magnetic flux, and energy at the magnetopause boundary because of strong flow shears on the dayside magnetopause boundary due, in part, to partial corotation of the magnetodisc (