The Chandrasekhar Mass Limit refers to the maximum mass of a stable white dwarf star, which is approximately (solar masses). This limit is a result of the principles of quantum mechanics and the effects of electron degeneracy pressure, which counteracts gravitational collapse. When a white dwarf's mass exceeds this limit, it can no longer support itself against gravity. This typically leads to the star undergoing a catastrophic collapse, potentially resulting in a supernova explosion or the formation of a neutron star. The Chandrasekhar Mass Limit plays a crucial role in our understanding of stellar evolution and the end stages of a star's life cycle.
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