<Ul> <Li> Granules </Li> <Li> Sunspot </Li> <Li> Photosphere </Li> <Li> Chromosphere </Li> <Li> Convection zone </Li> <Li> Radiation zone </Li> <Li> Tachocline </Li> <Li> Solar core </Li> <Li> Corona </Li> <Li> Flare </Li> <Li> Prominence </Li> <Li> Solar wind </Li> </Ul> <P> The solar wind is a stream of charged particles released from the upper atmosphere of the Sun, called the corona . This plasma consists of mostly electrons, protons and alpha particles with kinetic energy between 0.5 and 10 keV . Embedded within the solar - wind plasma is the interplanetary magnetic field . The solar wind varies in density, temperature and speed over time and over solar latitude and longitude . Its particles can escape the Sun's gravity because of their high energy resulting from the high temperature of the corona, which in turn is a result of the coronal magnetic field . </P> <P> At a distance of more than a few solar radii from the Sun, the solar wind is supersonic and reaches speeds of 250 to 750 kilometers per second . The flow of the solar wind is no longer supersonic at the termination shock . The Voyager 2 spacecraft crossed the shock more than five times between 30 August and 10 December 2007 . Voyager 2 crossed the shock about a billion kilometers closer to the Sun than the 13.5 - billion - kilometer distance where Voyager 1 came upon the termination shock . The spacecraft moved outward through the termination shock into the heliosheath and onward toward the interstellar medium . Other related phenomena include the aurora (northern and southern lights), the plasma tails of comets that always point away from the Sun, and geomagnetic storms that can change the direction of magnetic field lines . </P>

What is the continuous stream of particles that are blown away from the solar corona