Depth of Jupiter’s Zonal Flow under the “Shallow-wind” Assumption

Abstract

Abstract In this article, the depth of Jupiter’s zonal flow in the molecular-hydrogen region is for the first time explored in the context of the so-called “shallow-wind” scenario, which means the internal zonal circulation is kinematically different from the fast atmospheric jet stream. A gravitationally constrained zonal flow of typical speed is adopted. The zonal flow is examined in the semiconducting region for its MHD interaction with Jupiter’s main magnetic field and the resulting ohmic dissipation. Our calculations indicate that the zonal flow in Jupiter might be permitted to reach downward to the radial location at , deeper than previous estimations obtained by assuming the fast cloud-top zonal wind extended straightforward into Jupiter’s interior. On the other hand, it is also concluded that Jupiter’s zonal flow likely cannot penetrate any deeper to where electrical conductivity is greater than ; though, fluid motion might be slow under the “shallow-wind” model assumption.