  Dwarf galaxies are known to exhibit an unusual richness in numbers of
globular clusters (GCs), property quantified by the specific frequency ($S_N$),
which is high for dwarf and giant elliptical galaxies, but with a minimum for
intermediate-mass galaxies. In this work we study the role that GC evolution
has in setting this trend, for which we use ${\it N}$-body simulations to
evolve GCs in dwarf galaxies and quantify their disruption efficiency. We
selected five individual dwarf galaxies from a high-resolution cosmological
simulation, which includes GC formation and follow-up of their paths inside the
host galaxy. Then, the tidal history of each GC is coupled to NBODY6++GPU to
produce ${\it N}$-body models that account for both, the interaction of GCs
with their galactic environment and their internal dynamics. This results in a
GC mass loss parameterization to estimate dissolution times and mass loss rates
after a Hubble time. GC evolution is sensitive to the particular orbital
histories within each galaxy, but the overall result is that the amount of mass
that GC systems lose scales with the mass (and density) of the host galaxy,
i.e., the GC mass loss efficiency is lowest in low-mass dwarfs. After a 12 Gyr
evolution all simulated GC systems retain an important fraction of their
initial mass (up to 25%), in agreement with the high GC to field star ratios
observed in some dwarfs, and supports the scenario in which GC disruption
mechanisms play an important role in shaping the GC specific frequency in dwarf
galaxies.
