  The stability of satellites in the solar system is affected by the so-called
evection resonance. The moons of Saturn, in particular, exhibit a complex
dynamical architecture in which co-orbital configurations occur, especially
close to the planet where this resonance is present.
  We address the dynamics of the evection resonance, with particular focus on
the Saturn system, and compare the known behavior of the resonance for a single
moon to that of a pair of moons in co-orbital trojan configuration.
  We developed an analytic expansion of the averaged Hamiltonian of a trojan
pair of bodies, including the perturbation from a distant massive body. {The
analysis of the corresponding equilibrium points was restricted to the
asymmetric apsidal corotation solution of the co-orbital dynamics.} We also
performed numerical N-body simulations to construct dynamical maps of the
stability of the evection resonance in the Saturn system, and to study the
effects of this resonance under the migration of trojan moons caused by tidal
dissipation.
  The structure of the phase space of the evection resonance for trojan
satellites is similar to that of a single satellite, differing in that the
libration centers are displaced from their standard positions by an angle that
depends on the periastron difference $\varpi_2-\varpi_1$ and on the mass ratio
$m_2/m_1$ of the trojan pair.
  The interaction with the inner evection resonance may have been relevant
during the early evolution of the Saturn moons Tethys, Dione, and Rhea. In
particular, Rhea may have had trojan companions in the past that were lost when
it crossed the evection resonance, while Tethys and Dione may either have
retained their trojans or have never crossed the evection. This may help to
constrain the dynamical processes that led to the migration of these satellites
and to the evection itself.
