Everything about Photodisintegration totally explained
Photodisintegration is a physical process in which extremely high energy
gamma rays interact with an
atomic nucleus and cause it to enter an excited state, which immediately decays into two or more daughter nuclei. A simple example is when a single
proton or
neutron is effectively knocked out of the nucleus by the incoming gamma ray, and an extreme example is when the gamma ray induces a spontaneous
nuclear fission reaction. This process is essentially the reverse of
nuclear fusion, where lighter elements at high temperatures combine together forming heavier elements and releasing energy. Photodisintegration is
endothermic (energy absorbing) for atomic nuclei lighter than
iron and
exothermic (energy releasing) for atomic nuclei heavier than
iron. Photodisintegration is responsible for the
nucleosynthesis of at least some heavy, proton rich elements via
p-process which takes place in
supernovae.
In explosions of very large stars (250 or more times the mass of earth's
Sun), photodisintegration is a major factor in the
supernova event.
As the star reaches the end of its life, it reaches temperatures and pressures where photodisintegration's energy absorbing effects temporarily reduce pressure and temperature within the star's core.
This causes the core to start to collapse as energy is taken away by photodisintegration, and the collapsing core leads to the formation of a
black hole.
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