  In this work we analyze the orbital evolution and the dynamical stability in
the vicinity of the small Saturnian moons Aegaeon, Methone, Anthe and Pallene.
We numerically resolve the exact equations of motions to investigate the
orbital motion of thousands of test particles within and near to the domain of
the 7/6, 14/15, 10/11 mean motion resonances of Aegaeon, Methone and Anthe with
Mimas, respectively. We show that, for massless small moons, the orbits of
particles initially restricted to the resonant domains remain stable for at
least $10^4$ yr. We also conduct numerical simulations considering Aegaeon,
Methone, Anthe and Pallene as massive bodies. The results show that most
particles undergo significant perturbations in their orbital motions,
ultimately destabilizing in timescales of a few hundreds of years or even less
through collisions with the four small moons. In addition, we also simulate the
orbital evolution of test particles initially distributed in form of arc around
Aegaeon, Methone and Anthe. We show that the initial arcs are dynamically
eroded on timescales of hundreds of years, allowing us to constraint the
timescales for which gravitational forces operate to remove particles from the
observed arcs.
