What is the name of the critical mass at which white dwarfs may go supernova?

The Chandrasekhar Limit is the critical mass threshold for white dwarfs to undergo a type Ia supernova. This limit is approximately 1.4 times the mass of the Sun. When a white dwarf, which is the remnant of a star that has exhausted its nuclear fuel, accumulates mass from a companion star or via other means, it can approach this limit. At or above this mass, the pressure and temperature in the white dwarf's core become sufficient to ignite carbon fusion in a runaway reaction, leading to a dramatic explosion.

Understanding this limit is crucial in stellar astrophysics because type Ia supernovae serve as important tools in measuring cosmic distances and understanding the expansion of the universe. In contrast, the Schwarzschild Limit pertains to black holes, the Eddington Limit relates to the balance between radiation pressure and gravitational forces in stars, and the "Einstein Limit" is not a standard term in astrophysics.