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  2. List of states of matter - Wikipedia

    en.wikipedia.org/wiki/List_of_states_of_matter

    Helimagnetism: A state with spatially rotating magnetic order. Spin glass: A magnetic state characterized by randomness. Quantum spin liquid: A disordered state in a system of interacting quantum spins which preserves its disorder to very low temperatures, unlike other disordered states.

  3. 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 ...

  4. State of matter - Wikipedia

    en.wikipedia.org/wiki/State_of_matter

    A quantum Hall state gives rise to quantized Hall voltage measured in the direction perpendicular to the current flow. A quantum spin Hall state is a theoretical phase that may pave the way for the development of electronic devices that dissipate less energy and generate less heat. This is a derivation of the Quantum Hall state of matter.

  5. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    Sirius B, which is a white dwarf, can be seen as a faint point of light to the lower left of the much brighter Sirius A. A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter. A white dwarf is very dense: in an Earth sized volume, it packs a mass that is comparable to the Sun.

  6. 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 ...

  7. 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

  8. 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]

  9. Matter - Wikipedia

    en.wikipedia.org/wiki/Matter

    The demonstration by Subrahmanyan Chandrasekhar that white dwarf stars have a maximum allowed mass because of the exclusion principle caused a revolution in the theory of star evolution. [44] Degenerate matter includes the part of the universe that is made up of neutron stars and white dwarfs.