  The aim of this study is to simulate the slow mode structures in the Hermean
magnetosphere. We use a single fluid MHD model and a multipolar expansion of
the Northward displaced Hermean magnetic field, to perform simulations with
different solar wind parameter to foreseen the most favorable configuration for
the formation of slow modes, attending to the solar wind density, velocity,
temperature and the interplanetary magnetic field orientation. If the
interplanetary magnetic field is aligned with the Mercury-Sun direction, the
magnetic axis of Mercury in the Northward direction or the planet orbital
plane, slow mode structures are observed nearby the South pole. If the
orientation is in the Sun-Mercury or Northward directions, slow mode structures
are observed nearby the North pole, but smaller compared with the structures
near the South pole. Increase the density or the solar wind velocity avoids the
formation of slow modes structures, not observed for a dynamic pressure larger
than $6.25 \cdot 10^{-9}$ Pa in the case of a Northward interplanetary magnetic
field orientation, due to the enhancement of the bow shock compression. If the
solar wind temperature increases, the slow mode structures are wider because
the sonic Mach number is smaller and the bow shock is less compressed.
