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degeneracy pressure in a sentence

"degeneracy pressure" in Chinese  

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  • They therefore provide neutron degeneracy pressure to support a neutron star against collapse.
  • It's not really accurate that there are two kinds of degeneracy pressure.
  • This degeneracy pressure is responsible for keeping certain massive stars from collapsing due to gravity.
  • It is supported only by electron degeneracy pressure, causing it to be extremely dense.
  • The actual mechanism though which the degeneracy pressure arises is the momentum of the neutrons.
  • Degeneracy pressure keeps dense stars in equilibrium, independent of the thermal structure of the star.
  • The pressure ( called degeneracy pressure or Fermi pressure ) remains nonzero even at absolute zero temperature.
  • The limit for objects supported by ideal neutron degeneracy pressure is only 0.75 solar masses.
  • Only when a star is sufficiently massive to overcome the degeneracy pressure can it collapse into a singularity.
  • This in turn results in degeneracy pressure for fermions the strong resistance of fermions to compression into smaller volume.
  • It's difficult to see degeneracy pressure in a sentence .
  • Neutrons are capable of producing an even higher degeneracy pressure, neutron degeneracy pressure, albeit over a shorter range.
  • Neutrons are capable of producing an even higher degeneracy pressure, neutron degeneracy pressure, albeit over a shorter range.
  • The momentum of the fermions in the fermion gas nevertheless generates pressure, termed " degeneracy pressure ".
  • :: : Actually the degeneracy pressure can be expressed as a gradient of a potential in the mesoscopic limit.
  • However, in a white dwarf, the electron degeneracy pressure doesn't increase very quickly as mass increases.
  • The limit of neutron degeneracy pressure, analogous to the Chandrasekhar limit, is known as the Tolman Oppenheimer Volkoff limit.
  • Likewise, degenerate matter still has normal thermal pressure, but at extremely high densities, the degeneracy pressure usually dominates.
  • The high density scenario occurs in neutron starts, where there is a large degeneracy pressure, independent of nuclear forces.
  • In white dwarfs, which do not undergo nuclear fusion, an opposing force to gravity is provided by electron degeneracy pressure.
  • The neutrons resist further compression by the Pauli Exclusion Principle, in a way analogous to electron degeneracy pressure, but stronger.
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