In this paper,we report on our study of the trajectories of solar wind electrons reflected by lunar electric and magnetic fields through analysis of reflectivity and distribution under different conditions.Our calculations and simulations showed that the variations of both the magnetic field and surface potential play important roles in changing the directions of the traces of electrons.Furthermore,we were able to distinguish the changes resulting from these two variations through further analysis of the results.Thus,both the magnitude of the crustal field and the surface potential can be acquired from the data of satellites such as the Lunar Prospector.These findings could also contribute to the design and development of new devices in future lunar programs.
We study the interaction between the Moon and the solar wind through a three-dimensional MHD simulation.Three cases have been discussed in which the interplanetary magnetic field lies at 90,180,and 135 to the solar wind flow,respectively.A wake with low density and low pressure can always be formed behind the Moon.The plasma temperature and magnetic field are enhanced in the central wake,but the field strength is reduced in the surrounding region.A Mach cone is formed by rarefaction waves emanating from the limb.These rarefaction waves propagate via the fast magnetosonic mode with different velocities in different directions relative to the magnetic field.When the interplanetary magnetic field is not parallel to the solar wind flow,the wake shows some asymmetries,with an acceleration region turning up at the center.Finally,the results are compared with the observations by WIND spacecraft.Our calculations agree reasonably well with the observed values.
