White dwarfs are formed when massive stars exhaust their nuclear fuel and undergo gravitational collapse. The core of the star collapses under its own gravity, while the outer layers are expelled in a supernova explosion.

The Chandrasekhar Limit is the maximum mass a white dwarf can have before its electron degeneracy pressure can no longer support its own gravity. If the mass of a white dwarf exceeds the Chandrasekhar Limit, it will collapse into a neutron star.

White dwarfs are supported against gravitational collapse by electron degeneracy pressure. This pressure arises from the Pauli exclusion principle, which prevents electrons from occupying the same quantum state.

White dwarfs are extremely dense objects, with masses comparable to that of the Sun but volumes comparable to that of the Earth.

White dwarfs are hot objects, but their temperatures are much lower than those of stars. This is because they no longer undergo nuclear fusion and rely on residual heat from their formation.

White dwarfs gradually cool over time as they radiate their heat into space. Eventually, they will reach a state where they are no longer visible and are known as black dwarfs.

J0023+0923 is a white dwarf with a mass of 2.15 solar masses. It is the most massive white dwarf known to date and is located in the constellation Pisces.

Sirius B is a white dwarf located 8.6 light-years from Earth in the constellation Canis Major. It is the closest white dwarf to Earth and is a companion star to the bright star Sirius.

White dwarfs can accrete matter from a companion star through a process known as Roche lobe overflow. If the mass of the white dwarf exceeds the Chandrasekhar Limit, it can trigger a Type Ia supernova.

White dwarfs can release heavy elements during Type Ia supernova explosions. These explosions eject large amounts of material into the interstellar medium, enriching it with heavy elements.

White dwarfs are the end products of stellar evolution for low- to intermediate-mass stars. Studying white dwarfs provides valuable insights into the final stages of stellar evolution and the processes that lead to the formation of these compact objects.

White dwarfs can expel their outer layers, creating a glowing shell of gas known as a planetary nebula. This process occurs as the white dwarf sheds its mass due to strong stellar winds or binary interactions.

White dwarfs can merge with other white dwarfs, forming a double degenerate binary system. These systems are important progenitors of Type Ia supernovae and gravitational wave sources.

White dwarfs can accrete matter from a companion star through Roche lobe overflow. This process can lead to the formation of cataclysmic variables, which are binary systems that exhibit sudden outbursts due to the accretion of matter onto the white dwarf.