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The aim of this research is to simulate the interaction of the solar windwith the magnetic field of Mercury and to study the particle fluxes between themagnetosheath and the planet surface. We simulate the magnetosphere structureusing the open source MHD code PLUTO in spherical geometry with a multipolarexpansion of the Hermean magnetic field (Anderson, B. J. et al, 2012). Weperform two simulations with realistic solar wind parameters to study theproperties of a plasma stream originated in the reconnection region between theinterplanetary and the Hermean magnetic field. The plasma precipitates alongthe open magnetic field lines to the planet surface showing a fast expansion,rarefaction and cooling. The plasma stream is correlated with a flattening ofthe magnetic field observed by MESSENGER due to the adjacency of thereconnection region where the solar wind is injected to the innermagnetosphere.

Plasma streams in the Hermean dayside magnetosphere: solar wind injection through the reconnection region