  The aim of this paper is to study the plasma flows on the Mercury surface for
different interplanetary magnetic field orientations on the day side of the
planet. We use a single fluid MHD model in spherical coordinates to simulate
the interaction of the solar wind with the Hermean magnetosphere for six solar
wind realistic configurations with different magnetic field orientations:
Mercury-Sun, Sun-Mercury, aligned with the magnetic axis of Mercury (Northward
and Southward) and with the orbital plane perpendicular to the previous cases.
In the Mercury-Sun (Sun-Mercury) simulation the Hermean magnetic field is
weakened in the South-East (North-East) of the magnetosphere leading to an
enhancement of the flows on the South (North) hemisphere. For a Northward
(Southward) orientation there is an enhancement (weakening) of the Hermean
magnetic field in the nose of the bow shock so the fluxes are reduced and
drifted to the poles (enhanced and drifted to the equator). If the solar wind
magnetic field is in the orbital plane the magnetosphere is tilted to the West
(East) and weakened at the nose of the shock, so the flows are enhanced and
drifted to the East (West) in the Northern hemisphere and to the West (East) in
the Southern hemisphere.
