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<p><b>New page</b></p><div>[[File:Sirius_A_and_B_Hubble_photo.editted.PNG|Sirius A and B Hubble photo.editted|thumb]] '''White dwarf''' stars are the remnants of [[low-mass]] and [[medium-mass]] stars that have exhausted their nuclear fuel. These stellar cores are primarily composed of [[electron-degenerate matter]], a state of matter arising from the Pauli exclusion principle, which states that two electrons cannot occupy the same quantum state at the same time. This principle provides a pressure that supports the white dwarf against gravitational collapse.<br />
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== Formation ==<br />
The formation of a white dwarf occurs at the end of a star's life cycle. Stars like the [[Sun]] spend most of their lives converting hydrogen into helium in their cores through nuclear fusion, a phase known as the main sequence. Once the hydrogen is depleted, stars not massive enough to fuse helium into heavier elements will shed their outer layers, creating a [[planetary nebula]], and leave behind a white dwarf.<br />
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== Characteristics ==<br />
White dwarfs have masses up to 1.4 times that of the Sun, a limit known as the [[Chandrasekhar limit]]. Beyond this limit, the white dwarf would collapse into a [[neutron star]] or a [[black hole]]. Despite their mass, white dwarfs have a small radius, similar to that of Earth, leading to very high densities.<br />
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The temperature of a white dwarf at formation can exceed 100,000 Kelvin, causing it to emit strongly in ultraviolet and visible light. Over billions of years, a white dwarf will cool and fade to become a [[black dwarf]], a theoretical state that the universe is not old enough to contain any examples of.<br />
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== Observations and Importance ==<br />
White dwarfs are important to astronomers as they serve as one of the few observable endpoints of stellar evolution. The most famous white dwarf is Sirius B, part of the [[Sirius]] binary system, which was one of the first white dwarfs to be discovered. Observing white dwarfs allows astronomers to understand more about the life cycle of stars, the physics of degenerate matter, and the future of our own Sun.<br />
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== White Dwarfs in Binary Systems ==<br />
In binary systems, white dwarfs can accrete material from a companion star. This process can lead to a variety of phenomena, including [[nova]]e and, if the white dwarf approaches the Chandrasekhar limit, a Type Ia [[supernova]], which is critical for measuring cosmic distances.<br />
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== Future Research ==<br />
Research on white dwarfs continues to evolve, with astronomers using them to study topics such as [[stellar evolution]], [[cosmology]], and the properties of matter under extreme conditions. The ongoing discovery and observation of white dwarfs in binary systems, and the potential for these systems to produce gravitational waves, also presents an exciting frontier for future research.<br />
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[[Category:Astronomy]]<br />
[[Category:Stars]]<br />
[[Category:White dwarfs]]<br />
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