  The Fornax dwarf spheroidal galaxy (dSph) represents a challenge for some
globular cluster (GC) formation models, because an exceptionally high fraction
of its stellar mass is locked in its GC system. In order to shed light on our
understanding of GC formation, we aim to constrain the amount of stellar mass
that Fornax has lost via tidal interaction with the Milky Way (MW). Exploiting
the flexibility of effective multi-component $N$-body simulations and relying
on state-of-the-art estimates of Fornax's orbital parameters, we study the
evolution of the mass distribution of the Fornax dSph in observationally
justified orbits in the gravitational potential of the MW over 12 Gyr. We find
that, though the dark-matter mass loss can be substantial, the fraction of
stellar mass lost by Fornax to the MW is always negligible, even in the most
eccentric orbit considered. We conclude that stellar-mass loss due to tidal
stripping is not a plausible explanation for the unexpectedly high stellar mass
of the GC system of the Fornax dSph and we discuss quantitatively the
implications for GC formation scenarios.
