What is a Pair-Instability Supernova?
A pair-instability supernova is a special type of supernova, or stellar explosion, occurring only in stars which are very massive (between 130 and 250 solar masses), have low to moderate rotation rates, and low metallicity (primarily made of hydrogen and helium). In a pair-instability supernova, the star’s core is so extremely energetic that collisions between gamma rays and atomic nuclei result in the spontaneous creation of electron-positron pairs, siphoning away much of the thermal energy and leading to a drop in pressure. This pressure drop results in the star partially collapsing due to gravity. Collapse regions are quickly superheated to extreme temperatures and pressures, causing the rapid fusion of atomic nuclei and tremendous energy release. The resulting thermal energy is so huge that it blows the star completely apart, leaving behind nothing behind. All other supernovae leave behind black hole or neutron star remnants. Pair-instability supernovae are thought to be rare today
