What is Solar Wind?

Edited by Doron Tal, 4X4XM

Solar wind refers to a stream of charged particles, primarily electrons and protons, that are continuously emitted by the Sun's corona, which is the outermost layer of the Sun's atmosphere.

These particles are ejected from the Sun at high speeds, ranging from 400 to 800 km/s (about 1 to 2.5 million miles per hour) and travel through the solar system, interacting with the magnetic fields of planets, asteroids, and comets.

An illustration of the solar wind and the Earth's magnetosphere that shows how the solar wind rearranges the magnetosphere. It compresses the magnetic field on the side facing the sun while elongating it on the opposite end.

The solar wind is a major factor affecting the space environment around the Earth and other planets, and it can cause phenomena such as auroras, geomagnetic storms, and radiation belts. It also plays a crucial role in the dynamics of the solar system, including the interaction between the Sun and its planets, and the evolution of planetary atmospheres and surfaces.

You may find more detailed information in the main webpage, here. See also an index for HF Radio Propagarion.