Solar Wind: Mass of ionized gas emitted to space by the sun. Plays a role in the formation of auroras. It is caused by the hot solar corona, which is the outermost layer of the solar atmosphere, expanding into space. The solar wind differs in density, warmth, and velocity over time and over solar latitude and longitude. Its particles can flee the Sun’s gravity because of their lofty force resulting from the lofty temperature of the corona, which in turn is a consequence of the coronal magnetic field.
The velocity of the solar wind is superior over coronal holes, reaching speeds of up to 500 miles (800 kilometers) per second. The warmth and mass of coronal holes are low, and the magnetic field is feeble, so the field lines are open to space. These holes happen at the poles and low latitudes and attain their largest when movement on the sun is at its least. Temperatures in the fast wind can reach up to 1 million degrees F (800,000 C).