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Cosmology and Particle Physics

  • Chapter
The Early Universe

Part of the book series: NATO ASI Series ((ASIC,volume 219))

Abstract

In the past five years or so progress in both elementary particle physics and in cosmology has become increasingly dependent upon the interplay between the two disciplines. On the particle physics side, the SU(3) c × SU(2) L × U(1)Y model seems to very accurately describe the interactions of quarks and leptons at energies below, say, 103 GeV. At the very least, the so-called standard model is a satisfactory, effective low energy theory. The frontiers of particle physics now involve energies of much greater than 103 GeV—energies which are not now available in terrestrial accelerators, nor are ever likely to be available in terrestrial accelerators. For this reason particle physicists have turned both to the early Universe with its essentially unlimited energy budget (up to 1019 GeV) and high particle fluxes (up to 10107cm-2s-1), and to various unique, contemporary astrophysical environments (centers of main sequence stars where temperatures reach 108 K, neutron stars where densities reach 1014 – 1015gcm-3, our galaxy whose magnetic field can impart 1011 GeV to a Dirac magnetic charge, etc.) as non-traditional laboratories for studying physics at very high energies and very short distances.

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  1. NASA/Fermilab Astrophysics Center, Fermi National Accelerator Laboratory, Batavia, 60510, Illinois, USA

    Michael S. Turner

  2. Departments of Physics and Astronomy and Astrophysics Enrico Fermi Institute, The University of Chicago, Chicago, 60637, Illinois, USA

    Michael S. Turner

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  1. Department of Physics, The University of British Columbia, Vancouver, Canada

    W. G. Unruh  & G. W. Semenoff  & 

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Turner, M.S. (1988). Cosmology and Particle Physics. In: Unruh, W.G., Semenoff, G.W. (eds) The Early Universe. NATO ASI Series, vol 219. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-4015-4_2

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