• Solar wind is a continuous stream of charged particles, primarily protons and electrons, that are emitted from the Sun’s corona, the outermost layer of its atmosphere. 
  • The particles in the solar wind are mostly electrons, protons and alpha radiation, but there are also trace amounts of heavy ions and atomic nuclei including carbon, nitrogen, oxygen, and some heavier metals.
  • In addition to the continuous flow of solar wind, the Sun occasionally releases large bursts of charged particles in a single event, known as coronal mass ejections (CMEs). These eruptions can cause geomagnetic storms in Earth’s surrounding environment, which are associated with the stunning aurora displays.
• The solar wind extends throughout the solar system, reaching well beyond Pluto’s orbit, creating a vast “bubble” known as the heliosphere.
• The closest boundary of the heliosphere is about 100 AU out from the sun, according to an ESA statement. 
  • The heliosphere acts as a protective shield, defending us against cosmic rays consisting of energetic particles that can damage living cells
• While the solar wind continuously flows from the Sun, its characteristics—such as density and speed—fluctuate over the Sun’s 11-year activity cycle. Throughout this cycle, sunspot numbers, radiation levels, and the ejected material vary between the solar maximum and solar minimum. These changes influence the properties of the solar wind, including its magnetic field strength, travel speed, temperature, and density.

Effects of Solar Wind:

• The solar wind is a constant flow of protons and electrons emitted from the Sun’s outermost layer, the corona. When this wind reaches Earth, it sends a surge of charged particles into the magnetosphere, traveling along Earth’s magnetic field lines toward the poles. The interaction of these particles with Earth’s atmosphere can create luminous aurora displays near the polar regions.
• A strong solar wind can disrupt power grids, satellites, and communication systems.