* White Dwarf Stability: White dwarfs are incredibly dense objects composed primarily of degenerate electrons. The pressure exerted by these electrons counteracts the inward pull of gravity, keeping the star stable.
* Chandrasekhar Limit: The Chandrasekhar Limit represents the maximum mass a white dwarf can hold before this electron degeneracy pressure becomes insufficient to resist gravity.
* Collapse: When the mass exceeds this limit, the electrons are forced to combine with protons, forming neutrons and releasing neutrinos. This process causes the white dwarf to collapse catastrophically, releasing immense energy.
* Neutron Star Formation: The collapsed core becomes incredibly dense, forming a neutron star. These stars are only a few kilometers in diameter but contain a mass greater than our sun. They are supported by the degeneracy pressure of neutrons.
* Supernova: The collapse of the white dwarf can trigger a Type Ia supernova, one of the brightest events in the universe. This explosion releases massive amounts of energy and heavy elements, enriching the interstellar medium.
In summary, reaching the Chandrasekhar Limit signifies the end of a white dwarf's life and the beginning of a dramatic transformation into a neutron star, accompanied by a powerful supernova explosion.
