Limits on the Cosmic Baryon Density

  • Hubert Reeves
Chapter
Part of the NATO ASI Series book series (NSSB, volume 228)

Abstract

The astrophysical importance of the Q-H phase transition comes from the fact that, below the critical temperature, it may induce in the cosmic fluid baryon density inhomogeneities, together with inhomogeneities in the ratio of neutrons to protons. These inhomogeneities could later modify the Big Bang nucleosynthesis yields of the four cosmological nuclides: D, 3He, 4He, 7Li, over the values obtained in the case of the Standard Big-Bang (homogeneous density).

Keywords

Critical Temperature Baryon Number String Tension Baryonic Density Chiral Transition 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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Copyright information

© Plenum Press, New York 1990

Authors and Affiliations

  • Hubert Reeves
    • 1
  1. 1.Service d’Astrophysique, Institut d’Astrophysique de ParisC.E.N. SaclayGif sur YvetteFrance

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