Solar phenomena move about and can travel at a few hundred meters per second when they first appear. The solar wind is a stream of plasma released from the Sun's upper atmosphere. It consists of mostly electrons and protons with energies usually between 1.5 and 10 keV. The stream of particles varies in density, temperature and speed over time and over solar longitude. These particles can escape the Sun's gravity because of their high energy. The solar wind is divided into the slow solar wind and the fast solar wind. The slow solar wind has a velocity of about , a temperature
Relativistic plasma light. (About 10% of protons would have formula_3 at a temperature of 481 MeV - 5.6 TK.) Still higher energies are necessary to achieve a quark–gluon plasma. The primary changes in a plasma's behavior as it approaches the relativistic regime is slight modifications to the equations which describe a non-relativistic plasma and to collision and interaction cross sections. The equations may also need modifications to account for pair production of electron-positron pairs (or other particles at the highest temperatures). A plasma double layer with a large potential drop and layer separation, may accelerate electrons to relativistic velocities, and produce synchrotron