The sun, a searing hot sphere of gas primarily composed of hydrogen and helium, boasts surface and outer atmospheric temperatures ranging from 10,000 to 3.6 million degrees Fahrenheit on its surface and its atmosphere's outermost layer. This intense heat causes the sun to continuously emit a stream of plasma, made up of charged subatomic particles—mainly protons and electrons. These particles, possessing significant energy, escape the sun's gravitational pull and drift into space as solar wind. Understanding how charged particles interact with other transient eruptions of energy from the sun can help scientists study cosmic rays emitted in supernova explosions.