White Dwarfs are formed when stars of low to intermediate mass exhaust their nuclear fuel and undergo gravitational collapse, leading to the expulsion of their outer layers.

White Dwarfs typically have masses ranging from 0.1 to 1.4 Solar Masses, which is the Chandrasekhar Limit, beyond which they undergo further collapse to form Neutron Stars or Black Holes.

White Dwarfs primarily consist of Carbon and Oxygen, as they have exhausted their Hydrogen and Helium fuel through nuclear fusion processes.

White Dwarfs are incredibly dense, with masses comparable to the Sun but compressed into a volume similar to Earth or even smaller.

If a White Dwarf exceeds the Chandrasekhar Limit, it undergoes a sudden collapse, leading to the formation of a Neutron Star. This process is known as a Type Ia Supernova.

White Dwarfs primarily emit energy through thermal radiation, as they have exhausted their nuclear fuel and rely on their residual heat to sustain their luminosity.

White Dwarfs have surface temperatures ranging from 30,000 Kelvin to over 100,000 Kelvin, making them extremely hot despite their small size.

When a White Dwarf accretes material from a companion star, it can undergo a sudden outburst, known as a Nova. This occurs due to the release of energy as the accreted material undergoes nuclear fusion on the surface of the White Dwarf.

A binary system consisting of a White Dwarf and a Red Giant is known as a Cataclysmic Variable. These systems are characterized by periodic outbursts due to the transfer of mass from the Red Giant to the White Dwarf.

The first discovered White Dwarf was Sirius B, the companion star to the brightest star in the night sky, Sirius. It was identified as a White Dwarf in 1862 by the American astronomer Alvan Graham Clark.

A White Dwarf with a strong magnetic field is known as a Magnetic White Dwarf. These objects exhibit unique characteristics, such as rapid rotation and the emission of high-energy radiation.

White Dwarfs gradually cool and fade over time through the emission of thermal radiation. As they lose heat, their luminosity decreases, and they eventually become faint and difficult to detect.

A White Dwarf that is surrounded by a planetary nebula is known as the Central Star. Planetary nebulae are formed when the outer layers of a star are expelled during its final stages of evolution, revealing the hot core, which is the White Dwarf.

A binary system consisting of two White Dwarfs is known as a Double White Dwarf System. These systems are important for studying the evolution of White Dwarfs and the potential for mergers and supernovae.

The closest White Dwarf to Earth is Sirius B, located approximately 8.6 light-years away. It is the companion star to Sirius, the brightest star in the night sky.