Supernova

A supernova (plural supernovae), is an exploding variable star object, that reaches a maximum brightness at about the magnitude of an entire galaxy. Historically the supernovae were regarded as novae stars, but in the early 20th century it was discovered that the supernovae were much brighter by average about 10000 times the luminosity of a nova. Unlike the novae, who explode by termonuclear explosions of accreted matter, the supernovae are ignited by a collapse of an electron degenerate star core or a white dwarf over the mass limit termed the Chandrasekhar limit of 1.4 sun masses. This degenerate object then implodes to a neutron star, but rebound and photodissociation processes also causes the outer parts of the star to explode violently, causing the supernova brightness rise.

Physics

Unlike stars with less mass, stars with more than five times the mass of our sun can continue to burn each element synthesised in turn, hydrogen, helium, then carbon, oxygen, silicon and so forth until they are left with iron.

Nuclear binding energy per nucleon. Note iron-56 at the peak in the middle.

Due to a phenomenon known as nuclear binding energy, nucleons such as protons and neutrons will weigh a little less when they are bound in a nucleus than when they are by themselves. This mass deficiency is different from element to element, with hydrogen having a very high deficiency. Iron has the lowest deficiency of all elements, and will not release energy when fusioned. Instead, it draws thermal energy from the core leaving the star without energy to resist the force of gravity. This results in a collapse. The star can collapse in about 15 seconds, which is extremely fast. During the collapse of the star, the density of the materials increases and elements heavier than iron are produced.

Stars between 5 and 8 times that of our sun will collapse until they detonate in a catastrophic supernova explosion forming a neutron star.

What actually takes place is unclear. One explanation is that after having consumed their fuel, their overall energy level declines with the end of exothermic nuclear burning and they are unable to resist the forces of gravity. Their iron core collapses under gravitational forces until it is so dense it reaches nuclear densities and rebounds. As it rebounds it generates an outwardly propagating shock wave and a burst of neutrinos on the order of 10⁵³ ergs. The resultant explosion ejects the stellar envelope with a kinetic energy of 10⁵¹ ergs at a velocity of 10⁴ km s⁻¹.

In the process of the explosion elements heavier than nickel and iron are synthesised. The radioactive decay of ⁵⁶Ni and ⁵⁶Co create the energy to produce long-term optical light, reaching a luminosity in the range of 10⁴² to 10⁴³ erg s^-1 about 10-20 days after the explosion.

Stars with masses that exceed 10 times that of our sun collapse with such force that even a neutron star cannot resist the pressure of the collapsing star and the supernova creates a black hole.