Interaction of solar wind with magnetosphere of Venus

Nonuniformity in the structure of the solar corona and the transience of its processes determine a nonuniformity and fleetingness in the properties of solar wind, the medium in which the planets exist. The velocity and concentration of interplanetary plasma and the size and direction of the interplanetary magnetic field may therefore vary substantially. The density of solar wind is very low and its magnetic field quite weak. How then do the planets react to such an ephemeral phenomenon? It turns out that the interaction of atmospheres, ionospheres and the magnetic fields of the individual planets with solar wind and the interplanetary magnetic field comprise a special area of planetary physics which is quite significant. The initial discoveries in this sphere were made, naturally, with respect to the Earth. The Earth as a strong magnetic field. It was established that solar wind meets this obstacle as it nears our planet and skirts around it. As a result, the solar wind seemingly draws lines of force of the Earth's magnetic field out away from the Sun, creating a so-called magnetospheric tail hundreds of thousands of kilometers in length and about 200,000 km in cross section.