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  2. Chandrasekhar's white dwarf equation - Wikipedia

    en.wikipedia.org/wiki/Chandrasekhar's_white_dwarf...

    From the quantum statistics of a completely degenerate electron gas (all the lowest quantum states are occupied), the pressure and the density of a white dwarf are calculated in terms of the maximum electron momentum standardized as = /, with pressure = and density =, where

  3. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    White dwarfs with hydrogen-poor atmospheres, such as WD J2147–4035, are less affected by CIA and therefore have a yellow to orange color. [80] [77] The white dwarf cooling sequence seen by ESA's Gaia mission. White dwarf core material is a completely ionized plasma – a mixture of nuclei and electrons – that is

  4. Future of an expanding universe - Wikipedia

    en.wikipedia.org/.../Future_of_an_expanding_universe

    The universe will become extremely dark after the last stars burn out. Even so, there can still be occasional light in the universe. One of the ways the universe can be illuminated is if two carbon–oxygen white dwarfs with a combined mass of more than the Chandrasekhar limit of about 1.4 solar masses happen

  5. Compact object - Wikipedia

    en.wikipedia.org/wiki/Compact_object

    As they cool they will redden and dim until they eventually become dark black dwarfs. White dwarfs were observed in the 19th century, but the extremely high densities and pressures they contain were not explained until the 1920s. The equation of state for degenerate matter is "soft", meaning that adding more mass will result in a smaller object ...

  6. Electron degeneracy pressure - Wikipedia

    en.wikipedia.org/wiki/Electron_degeneracy_pressure

    In white dwarf stars, the positive nuclei are completely ionized – disassociated from the electrons – and closely packed – a million times more dense than the Sun. At this density gravity exerts immense force pulling the nuclei together. This force is balanced by the electron degeneracy pressure keeping the star stable. [4]

  7. Universal wavefunction - Wikipedia

    en.wikipedia.org/wiki/Universal_wavefunction

    Hugh Everett's universal wavefunction supports the idea that observed and observer are all mixed together: . If we try to limit the applicability so as to exclude the measuring apparatus, or in general systems of macroscopic size, we are faced with the difficulty of sharply defining the region of validity.

  8. List of states of matter - Wikipedia

    en.wikipedia.org/wiki/List_of_states_of_matter

    Quantum anomalous Hall state: A state which has a quantized Hall resistance even in the absence of external magnetic field. Topological insulator: a material whose interior behaves as an electrical insulator while its surface behaves as an electrical conductor. Fractional Chern insulator: A generalization of fractional quantum Hall state to ...

  9. Chandrasekhar–Eddington dispute - Wikipedia

    en.wikipedia.org/wiki/Chandrasekhar–Eddington...

    The remaining material forms a star in a very dense state. [2] One of the three white dwarfs, Sirius B, a companion to Sirius, was discovered by Walter Sydney Adams after a suggestion by Arthur Eddington to use the relativistic Doppler effect as predicted by special relativity. [2]