  The aim of the present study is to simulate the interaction between the solar
wind and the Hermean magnetosphere. We use the MHD code PLUTO in spherical
coordinates with an axisymmetric multipolar expansion of the Hermean magnetic
field, to perform a set of simulations with different interplanetary magnetic
field orientations and intensities. We fix the hydrodynamic parameters of the
solar wind to study the distortions driven by the interplanetary magnetic field
in the topology of the Hermean magnetosphere, leading to variations of the mass
and energy deposition distributions, the integrated mass deposition, the oval
aperture, the area covered by open magnetic field lines and the regions of
efficient particle sputtering on the planet surface. The simulations show a
correlation between the reconnection regions and the local maxima of plasma
inflow and energy deposition on the planet surface.
