  In anticipation of improved observational data for Jupiter's gravitational
field from the Juno spacecraft, we predict the static tidal response for a
variety of Jupiter interior models based on ab initio computer simulations of
hydrogen-helium mixtures. We calculate hydrostatic-equilibrium gravity terms
using the non-perturbative concentric Maclaurin Spheroid (CMS) method that
eliminates lengthy expansions used in the theory of figures. Our method
captures terms arising from the coupled tidal and rotational perturbations,
which we find to be important for a rapidly-rotating planet like Jupiter. Our
predicted static tidal Love number $k_2 = 0.5900$ is $\sim$10\% larger than
previous estimates. The value is, as expected, highly correlated with the zonal
harmonic coefficient $J_2$, and is thus nearly constant when plausible changes
are made to interior structure while holding $J_2$ fixed at the observed value.
We note that the predicted static $k_2$ might change due to Jupiter's dynamical
response to the Galilean moons, and find reasons to argue that the change may
be detectable, although we do not present here a theory of dynamical tides for
highly oblate Jovian planets. An accurate model of Jupiter's tidal response
will be essential for interpreting Juno observations and identifying tidal
signals from effects of other interior dynamics in Jupiter's gravitational
field.
