# Chandrasekhar Limit
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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.
14 | Chandrasekhar Limit & White Dwarf Stars
Indian scientist Subrahmanyan Chandrasekhar and his great achievement Chandrasekhar Limit has helped us to predict the fate of the stars, we get to know one as we call White Dwarf Stars. Keywords: Subrahmanyan Chandrasekhar, C.V.Raman, White Dwarfs, Red Giant, Red Supergiant, Chandrasekhar Limit, B…
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Supernova
Transcript: A supernova is the violently explosive death of a star with the corresponding release of radiant energy, a flood of neutrinos, and the creation and ejection of heavy elements into space, the most spectacular phenomena in astronomy. Supernovae can occur in two basically different ways. …
Supernova
Transcript: Consider a binary system where a giant or a supergiant star is in orbit around a white dwarf and where a mass transfer between the lobes pushes the white dwarf over the Chandrasekhar limit. At this point the white dwarf collapses catastrophically to form either a neutron star or a blac…
Chandrashekar Limit
Transcript: White dwarfs cannot have a larger mass than about 1.4 times the mass of the Sun because above this mass the white dwarf structure becomes unstable; gravity overcomes the degeneracy pressure of the electrons and further collapse occurs. This is called the Chandrasekhar Limit, and it app…
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Transcript: When a massive star dies the supernova that results can rival an entire galaxy in brightness, so it can be seen to a very large distance, a billion lightyears or more. When a single massive star dies it does not do so in a well regulated way, but the supernovae that result from a binar…
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