They are basically classified according to their luminosities and spectral lines. Type II supernovas have lesser peaking of maxima in contrast to Type I supernovas. They also die abruptly. Maxima is equivalent to 10 billion luminosities. When it comes to spectral lines, Type I supernovas do not have hydrogen spectral lines while the Type II supernovas do.

Type II supernovas usually occur at the end of a super giant star’s life. They usually result from stars having more than 8 solar masses that are unable to transform into white dwarfs. At the end a star’s life, the fuels become exhausted and nuclear reactions ensues.

In the case of the type 2 supernova, there is an increased production of iron in the core from continuous nuclear fusion. The nuclear reactions resulted from of the early conversion of the core into helium which later initiated the production of the different elements resulting to a massive core. The mass that is produced, more than 1.44 solar masses, is so great that implosion will ensue. The mass is the so called Chandrasekhar limit. When this limit is exceeded, the shrinking core will have an extremely high temperature that will cause the formation of neutrinos and neutrons. The forces between the neutrons will cause the implosion to be directed outward, resulting in a massive shock wave capable of causing the supernova.

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Supernovas are explosions towards the end of the life of a star. They are classified as supernova I and II, depending on their solar luminosities. Type I supernova has a peaked maxima (about 10 billion luminosities) and then gradually disappears. Type I supernova is further divided into Type Ia and Type Ib based on the spectra it emits. All type I’s do not have hydrogen lines. Here we will focus on Type Ia which shows a silicone line.

White dwarfs are the end of most of stars. They are then supported by electron pressure because of their intense density. However, there is a certain limit, known as the Chandrasekhar limit, to which the electron pressure can support the electrons. When the Chandrasekhar limit is achieved, the white dwarf becomes a neutron star.

In the case of the type Ia supernova, a white dwarf in a slowly-rotating binary system (composed of two stars) can get more mass from its pair. Because of this, the limit is never achieved. The core of the star is left with increased temperature and pressure. When the star has approached to 1% of the limit, nuclear reactions occur that is not regulated by this kind of white dwarf unlike in other stars.

The core of the star becomes unstable and within seconds, the temperature peaks to billions of degrees, causing its particles to gain enough energy to dismantle the star resulting into a Type Ia supernova. When explosion occurs, it can be so bright that it can outshine other galaxies near it.

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