Type Ia Supernova

A Type Ia supernova is a type of supernova that occurs in binary systems in which one of the stars is a white dwarf. The other star can be anything from a giant star to an even smaller white dwarf. Physically, carbon–oxygen white dwarfs with a low rate of rotation are limited to below 1.44 solar masses. Beyond this "critical mass", they reignite and in some cases trigger a supernova explosion; this critical mass is often referred to as the Chandrasekhar mass, but is marginally different from the absolute Chandrasekhar limit, where electron degeneracy pressure is unable to prevent catastrophic collapse. If a white dwarf gradually accretes mass from a binary companion, or merges with a second white dwarf, the general hypothesis is that a white dwarf's core will reach the ignition temperature for carbon fusion as it approaches the Chandrasekhar mass.

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Breaking the Cosmic Silence: First Detection of Radio Waves From Type Ia Supernova

Astronomers Detect Radio Waves from Type Ia Supernova

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Hubble Observes Distant Remnant of Type Ia Supernova

Hubble Observes Distant Remnant of Type Ia Supernova

Chandra Observes Distant Remnant of Type Ia Supernova

HD 265435 Will Explode as Type Ia Supernova in 70 Million Years, Astronomers Say