Estimates of the mass distribution and dark-matter (DM) content of dwarf spheroidal galaxies (dSphs) are usually derived under the assumption that the effect of the tidal field of the host galaxy is negligible over the radial extent probed by kinematic data sets. We assess the implications of this assumption in the specific case of the Fornax dSph by means of N-body simulations of a satellite orbiting around the Milky Way. We consider observationally motivated orbits and tailor the initial distributions of the satellite's stars and DM to match, at the end of the simulations, the observed structure and kinematics of Fornax. In all our simulations the present-day observable properties of Fornax are not significantly influenced by tidal effects. The DM component is altered by the interaction with the Galactic field (up to 20 per cent of the DM mass within 1.6 kpc is lost.), but the structure and kinematics of the stellar component are only mildly affected even in the more eccentric orbit (more than 99 per cent of the stellar particles remain bound to the dwarf.). In the simulations that successfully reproduce Fornax's observables, the dark-to-luminous mass ratio within 1.6 kpc is in the range 5-6, and up to 16-18 if measured within 3 kpc.