Speaker
Description
We present a preliminary study of the interaction between the solar wind under supersonic and super-Alfvénic conditions in the lunar environment outside the Earth's magnetosphere using a three dimensional magnetohydrodynamic model that solves the ideal MHD-PRJ equations. The model incorporates observationally plasma parameters from upstream monitors (ACE, DSCVR, WIND) as input, allowing a physically consistent description of plasma conditions. The simulation captures the evolution of key parameters such as velocity, density and magnetic field, showing the formation of discontinuities, shock-like structures and a wake region downstream of the Moon. Preliminary results show that the model can reproduce plasma structures and can be extended to include additional physical processes.