We attempt to merge conceptually planetary wind models of Jupiter's outer magnetosphere with reconnection models of Jupiter's outer magnetosphere. Solar wind reconnection scaling arguments predict 2-4 AU for the length of the Jovian tail, consistent with that inferred from Jovian cosmic ray propagation arguments. Two conceivable limits of solar wind reconnection driven internal magnetospheric convection emerge, depending upon whether or not the centrifugally driven planetary wind transports magnetic flux radially outward.