  NASA's Juno mission recently reported Jupiter's high-degree (degree $\ell$,
azimuthal order $m$ $=4,2$) Love number $k_{42}=1.289\pm0.063$ ($1\sigma$), an
order of magnitude above the hydrostatic $k_{42}$ obtained in a nonrotating
Jupiter model. After numerically modeling rotation, the hydrostatic
$k_{42}=1.743\pm0.002$ is still $7\sigma$ away from the observation, raising
doubts about our understanding of Jupiter's tidal response. Here, we use
first-order perturbation theory to explain the hydrostatic $k_{42}$ result
analytically. We use a simple Jupiter equation of state ($n=1$ polytrope) to
obtain the fractional change in $k_{42}$ when comparing a rotating model with a
nonrotating model. Our analytical result shows that the hydrostatic $k_{42}$ is
dominated by the tidal response at $\ell=m=2$ coupled into the spherical
harmonic $\ell,m=4,2$ by the planet's oblate figure. The $\ell=4$ normalization
in $k_{42}$ introduces an orbital factor $(a/s)^2$ into $k_{42}$, where $a$ is
the satellite semimajor axis and $s$ is Jupiter's average radius. As a result,
different Galilean satellites produce a different $k_{42}$. We conclude that
high-degree tesseral Love numbers ($\ell> m$, $m\geq2$) are dominated by
lower-degree Love numbers and thus provide little additional information about
interior structure, at least when they are primarily hydrostatic. Our results
entail important implications for a future interpretation of the currently
observed Juno $k_{42}$. After including the coupling from the well-understood
$\ell=2$ dynamical tides ($\Delta k_2 \approx -4\%$), Jupiter's hydrostatic
$k_{42}$ requires an unknown dynamical effect to produce a fractional
correction $\Delta k_{42}\approx-11\%$ in order to fit Juno's observation
within $3\sigma$. Future work is required to explain the required $\Delta
k_{42}$.
