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  2. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    The degenerate matter that makes up the bulk of a white dwarf has a very low opacity, because any absorption of a photon requires that an electron must transition to a higher empty state, which may not be possible as the energy of the photon may not be a match for the possible quantum states available to that electron, hence radiative heat ...

  3. 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]

  4. 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

  5. Degenerate matter - Wikipedia

    en.wikipedia.org/wiki/Degenerate_matter

    Following the Pauli exclusion principle, there can be only one fermion occupying each quantum state. In a degenerate gas, all quantum states are filled up to the Fermi energy. Most stars are supported against their own gravitation by normal thermal gas pressure, while in white dwarf stars the supporting force comes from the degeneracy pressure ...

  6. Chandrasekhar limit - Wikipedia

    en.wikipedia.org/wiki/Chandrasekhar_limit

    White dwarfs resist gravitational collapse primarily through electron degeneracy pressure, compared to main sequence stars, which resist collapse through thermal pressure. The Chandrasekhar limit is the mass above which electron degeneracy pressure in the star's core is insufficient to balance the star's own gravitational self-attraction.

  7. 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]

  8. Quantum state - Wikipedia

    en.wikipedia.org/wiki/Quantum_state

    Quantum mechanics specifies the construction, evolution, and measurement of a quantum state. The result is a prediction for the system represented by the state. Knowledge of the quantum state, and the rules for the system's evolution in time, exhausts all that can be known about a quantum system.

  9. Bose–Einstein statistics - Wikipedia

    en.wikipedia.org/wiki/Bose–Einstein_statistics

    As the quantum concentration depends on temperature, most systems at high temperatures obey the classical (Maxwell–Boltzmann) limit, unless they also have a very high density, as for a white dwarf. Both Fermi–Dirac and Bose–Einstein become Maxwell–Boltzmann statistics at high temperature or at low concentration.