This process of collecting material from the partner star can lead to a larger catastrophic explosion. If the mass of the white dwarf increases past a certain point known as the Chandrasekhar limit (about 1.4 solar masses), its internal pressure (provided by electron degeneracy!) is unable to withstand its own gravity and it begins to collapse. During the collapse, the temperature rises enough for carbon to fuse, and it does so violently and almost instantaneously. The result is a carbon-detonation or Type Ia supernova. This type of supernova completely destroys the star, leaving nothing behind.