Solar wind is a stream of matter in interplanetary space. It makes up the greater part of the gases existing here.
The magnetic_field of the Sun's corona is so strong, that in some areas it can hold the hot eruptions of gas in the form of rings or arches. The magnetic field becomes weaker further out from the Sun, allowing a constant stream of protons, electrons and ions to escape into space. Because of the rotation of the Sun, the solar wind develops into a spiral shape here.
Solar wind is the reason for the formation of comets'_tails. The tail of gas is produced when charged molecules and atoms interact with the solar wind.
Samples of lunar rock taken by the Apollo missions have shown that traces of the solar wind are to be found on the Moon. Solar wind also contributes to the intensification of the polar_lights when it penetrates the Van_Allen_Belt and causes a charge surplus there.
