Supernova refers to a stellar explosion which produces more energy than a nova (Parker 12-23). It is extremely luminous, and it usually causes a burst of radiation which significantly outshines the entire galaxy. It then fades from viewing after several weeks or even months. During this interval, a supernova is a capable of producing as much energy as that the sun can produce on its expected life span (Parker 12-23). In addition, the explosion usually expels much or even all of the materials of the star at a velocity of 300000 kilometers per second. During this explosion, it drives a shock wave into the interstellar medium surrounding it. The shock wave then sweeps up the expanding gas shell as well as dust referred to as supernova remnant (Marschal 2-4). A supernova explosion releases a substantial amount of radio waves as well as X-rays. In addition, it also releases cosmic rays (Parker 12-23). A supernova explosion also releases majority of the heavy elements which make up the constituents of the solar system into the interstellar medium. A reliable research indicates that abundance of these heavy elements is greater than normal (Marschal 2-4). This implies that these elements do not form during the explosion as many may tend to argue. The supernova remnant shell continues to expand significantly until at an advanced age, where it then dissolves completely into the interstellar medium.

This supernova attained magnitude of 4.5 in just after few hours, making it visible with naked eyes (Parker 12-23).
There are two broad categories of supernovae. These are Type I and Type II. This classification is according to what they detonate (Parker 12-23). A type I supernova is usually three times brighter than a Type II supernova. In addition, unlike Type II, Type I contains no hydrogen lines and they usually expand about twice as rapidly as Type II. Type I supernova results from binary systems in which a white dwarf of carbon-oxygen becomes an accreting matter from a companion (Marschal 2-4).

Type II supernova, on the other hand, usually occurs at the end of a massive star lifetime, when its nuclear fuel becomes exhausted. This implies that it becomes no longer supported by the production of nuclear energy. If the star' core is massive enough, it will then collapse to become a Type II supernova (Parker 12-23). Before the 17th century, the number of recorded supernovae was only seven. One of the most famous supernovae is the Crab Nebula, whose remnants are still visible today.

Crab Nebula

The Crab Nebula is a supernova remnant as well as a pulsar wind nebula which is in the constellation of Taurus (Marschal 2-4).…