Zonnesteenwind

Zonnesteenwind, also known as solar wind, is a continuous stream of charged particles, primarily electrons and protons, that emanates from the Sun's upper atmosphere, the corona. This plasma flows outward through the solar system at high speeds, typically ranging from 300 to 800 kilometers per second. The existence of solar wind was first theorized in the 1950s and later confirmed by spacecraft observations.

The Sun's magnetic field plays a crucial role in shaping and guiding the solar wind. The constant thermal pressure from the corona, combined with the outward expansion driven by magnetic forces, propels these particles away from the Sun. The solar wind carries with it a portion of the Sun's magnetic field, forming the heliospheric magnetic field that permeates the entire solar system.

When the solar wind interacts with planetary magnetospheres, such as Earth's, it can cause spectacular phenomena like auroras. The charged particles are channeled along the magnetic field lines and collide with atmospheric gases, exciting them and causing them to emit light. The solar wind also influences the space environment of planets, affecting satellite operations and even contributing to atmospheric erosion on planets without strong magnetic fields. Its study is vital for understanding space weather and its potential impacts on technology and human space exploration.