  The new data delivered by NASA's Juno spacecraft significantly increase our
understanding of Jupiter's internal dynamics. The gravity data constrain the
depth of the zonal flows observed at cloud level and suggest that they slow
down considerably at a depth of about $0.96\,r_J$, where $r_J$ is the mean
radius at the one bar level. Juno's magnetometer reveals the planet's internal
magnetic field. We combine the new zonal flow and magnetic field models with an
updated electrical conductivity profile to assess the zonal wind induced dynamo
action, concentrating on the outer part of Jupiter's molecular hydrogen region
where the conductivity increases very rapidly with depth. Dynamo action remains
quasi-stationary and can thus reasonably be estimated where the magnetic
Reynolds number remains smaller than one, which is roughly the region above
$0.96\,r_J$. We calculate that the locally induced radial magnetic field
reaches rms values of about $10^{-6}\,$T in this region and may just be
detectable by the Juno mission. Very localized dynamo action and a distinct
pattern that reflects the zonal wind system increases the chance to disentangle
this locally induced field from the background field. The estimates of the
locally induced currents also allow calculating the zonal flow related Ohmic
heating and associated entropy production. The respective quantities remain
below new revised predictions for the total dissipative heating and total
entropy production in Jupiter for any of the explored model combinations. Thus
neither Ohmic heating nor entropy production offer additional constraints on
the depth of the zonal winds.
