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Line 21:
Line 21: − Sometimes white dwarfs, if they are in binary systems, may collide and fuse, forming a star that exceeds the Chandrasekhar limit and explode in a [[Supernova#Type_1a|type Ia supernova]].+
→Fate of White Dwarfs: my understanding is that 1a supernovas are not the result of a collision
As a white dwarf is no longer powered by thermonuclear fusion, all the light and heat generated is from remaining thermal energy. Thus, the star will very slowly cool over time into a hypothetical ''black dwarf'', where it can no longer emit light or heat in significant quantities. As the time period required for this to occur is longer than 13.7 billion years, no black dwarf is expected to exist yet. Even when the black dwarf state is reached, the stellar remnant itself is still expected to continue to exist indefinitely.
As a white dwarf is no longer powered by thermonuclear fusion, all the light and heat generated is from remaining thermal energy. Thus, the star will very slowly cool over time into a hypothetical ''black dwarf'', where it can no longer emit light or heat in significant quantities. As the time period required for this to occur is longer than 13.7 billion years, no black dwarf is expected to exist yet. Even when the black dwarf state is reached, the stellar remnant itself is still expected to continue to exist indefinitely.
A white dwarf that is part of a binary system may gradually draw in matter from its companion star. If it accumulates enough mass to exceed the Chandrasekhar limit it will explode in a [[Supernova#Type_1a|type Ia supernova]]. What remains is an even denser object known as a [[neutron star]].
==Internal structure of a White Dwarf==
==Internal structure of a White Dwarf==