  Aims: We aim to determine whether Jupiter's obliquity is bound to remain
exceptionally small in the Solar System, or if it could grow in the future and
reach values comparable to those of the other giant planets.
  Methods: The spin axis of Jupiter is subject to the gravitational torques
from its regular satellites and from the Sun. These torques evolve over time
due to the long-term variations of its orbit and to the migration of its
satellites. With numerical simulations, we explore the future evolution of
Jupiter's spin axis for different values of its moment of inertia and for
different migration rates of its satellites. Analytical formulas show the
location and properties of all relevant resonances.
  Results: Because of the migration of the Galilean satellites, Jupiter's
obliquity is currently increasing, as it adiabatically follows the drift of a
secular spin-orbit resonance with the nodal precession mode of Uranus. Using
the current estimates of the migration rate of the satellites, the obliquity of
Jupiter can reach values ranging from 6{\deg} to 37{\deg} after 5 Gyrs from
now, according to the precise value of its polar moment of inertia. A faster
migration for the satellites would produce a larger increase in obliquity, as
long as the drift remains adiabatic.
  Conclusions: Despite its peculiarly small current value, the obliquity of
Jupiter is no different from other obliquities in the Solar System: It is
equally sensitive to secular spin-orbit resonances and it will probably reach
comparable values in the future.
