  The Juno orbiter continues to collect data on Jupiter's gravity field with
unprecedented precision since 2016, recently reporting a non-hydrostatic
component in the tidal response of the planet. At the mid-mission perijove 17,
Juno registered a Love number $k_2=0.565\pm0.006$ that is $-4\pm1\%$
($1\sigma$) from the theoretical hydrostatic $k_2^{(hs)}=0.590$. Here we assess
whether the aforementioned departure of tides from hydrostatic equilibrium
represents the neglected gravitational contribution of dynamical tides. We
employ perturbation theory and simple tidal models to calculate a fractional
dynamical correction $\Delta k_2$ to the well-known hydrostatic $k_2$.
Exploiting the analytical simplicity of a toy uniform-density model, we show
how the Coriolis acceleration motivates the negative sign in the $\Delta k_2$
observed by Juno. By simplifying Jupiter's interior into a core-less,
fully-convective, and chemically-homogeneous body, we calculate $\Delta k_2$ in
a model following an $n=1$ polytrope equation of state. Our numerical results
for the $n=1$ polytrope qualitatively follow the behaviour of the
uniform-density model, mostly because the main component of the tidal flow is
similar in each case. Our results indicate that the gravitational effect of the
Io-induced dynamical tide leads to $\Delta k_2=-4\pm1\%$, in agreement with the
non-hydrostatic component reported by Juno. Consequently, our results suggest
that Juno obtained the first unambiguous detection of the gravitational effect
of dynamical tides in a gas giant planet. These results facilitate a future
interpretation of Juno tidal gravity data with the purpose of elucidating the
existence of a dilute core in Jupiter.
