  Many exoplanets have been observed close to their parent stars with orbital
periods of a few days. As for the major satellites of the Jovian planets, the
figure of these planets is expected to be strongly shaped by tidal forces.
However, contrarily to Solar System satellites, exoplanets may present high
values for the obliquity and eccentricity due to planetary perturbations, and
may also be captured in spin-orbit resonances different from the synchronous
one. Here we give a general formulation of the equilibrium figure of those
bodies, that makes no particular assumption on the spin and/or orbital
configurations. The gravity field coefficients computed here are well suited
for describing the figure evolution of a body whose spin and orbit undergo
substantial variations in time.
