The stream of charged particles given off from the Sun is called the solar wind. The solar wind consists primarily of protons (hydrogen nuclei) and electrons, with trace amounts of other ions and atomic nuclei. It is a continuous flow of plasma, which is a high-temperature, ionized gas composed of charged particles.
The solar wind originates from the outermost layer of the Sun's atmosphere, called the corona. The corona has an extremely high temperature and is highly ionized, with particles being accelerated to high speeds by the Sun's intense heat and magnetic activity. These charged particles then escape the Sun's gravitational pull and stream outward in all directions.
The solar wind has a significant impact on the Earth and other planets in the solar system. When it interacts with the Earth's magnetosphere, it can cause disturbances such as auroras (Northern and Southern Lights) and geomagnetic storms. The solar wind's effects can also influence the behavior of spacecraft, communication systems, and power grids on Earth.
Additionally, the solar wind interacts with the magnetic fields of other planets, affecting their atmospheres and magnetospheres. Understanding the properties and behavior of the solar wind is an important area of study in space physics and heliophysics.