  One of the leading scenarios for the formation of nuclear star clusters in
galaxies is related to the orbital decay of globular clusters (GCs) and their
subsequent merging, though alternative theories are currently debated. The
availability of high-quality data for GCs structural and orbital parameters
allow to test different nuclear star cluster formation scenarios. The Fornax
dwarf spheroidal (dSph) galaxy is the heaviest satellite of the Milky Way and
it is the only known dwarf spheroidal hosting 5 GCs, whereas there are no clear
signatures for the presence of a central massive black hole. For this reason,
it represents a suited place to study the orbital decay process in dwarf
galaxies. In this paper we model the future evolution of the Fornax GCs
simulating them and the host galaxy by means of direct $N$-body simulations.
Our simulations take in account also the gravitational field generated by the
Milky Way. We found that if the Fornax galaxy is embedded in a standard Cold
Dark Matter Halo, the nuclear cluster formation would be significantly hampered
by the high central galactic mass density. In this context, we discuss the
possibility that infalling GCs drive the flattening of the galactic density
profile, giving a possible alternative explanation to the so-called cusp/core
problem. Moreover, we briefly discuss the link between GC infall process and
the absence of massive black holes in the centre of dSphs.
