Numerical modeling of the solar wind interaction with Venus

The large-scale (global) interaction of the atmosphere of Venus with the surrounding medium is numerically simulated in the framework of 3-dimensional magnetohydrodynamics. The simulations are performed for the case of the interplanetary magnetic field perpendicular to the solar wind flow. The model reproduces several features of the interaction predicted by earlier theories and observations. The solar wind interaction with Venus is characterized by the mass loading of the solar wind with heavy oxygen ions which are produced by the photoionization of neutrals in the extensive ionosphere. This mass loading slows down the solar wind and ultimately leads to the formation of a magnetic barrier and a magnetotail. The location of the bow shock is barely affected by different values of the magnetic field strength.