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Dead stars could break one of physics' most famous limits
explained
The Chandrasekhar limit is the maximum mass of a stable white dwarf star. These stars resist gravitational collapse primarily through electron degeneracy pressure, compared to main sequence stars, which resist collapse through thermal pressure. The Chandrasekhar limit is the mass above which electron degeneracy pressure in the star's core is insufficient to balance the star's own gravitational self-attraction. The value of the Chandrasekhar limit depends upon the ratio of the number of electrons to nucleons (neutrons plus protons) in the star. For small stars this ratio is around 1/2 and the limit is about 1.44 M☉. The limit was named after Subrahmanyan Chandrasekhar who won the 1983 Nobel prize together with William Alfred Fowler for work on stellar models.
From Wikipedia: Chandrasekhar limit (CC BY-SA 4.0) ↗The usual limit, about 1.4 solar masses, underpins how Type Ia supernovae are used as cosmic distance markers, so heavier white dwarfs could change how we read the universe.
Subrahmanyan Chandrasekhar worked out his limit as a young man on a ship sailing from India to England.
Illustrative photo · Spacepotato, Public domain, via Wikimedia Commons
