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The Hot Big Bang and Beyond

Published online by Cambridge University Press:  25 May 2016

Michael S. Turner
Michael S. Turner*
Affiliation:
Departments of Physics and of Astronomy & Astrophysics, Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637-1433 NASA/Fermilab Astrophysics Center, Fermi National Accelerator Laboratory, Batavia, IL 60510-0500

Abstract

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The hot big-bang cosmology provides a reliable accounting of the Universe from about 10−2 sec after the bang until the present, as well as a robust framework for speculating back to times as early as 10−43 sec. Cosmology faces a number of important challenges; foremost among them are determining the quantity and composition of matter in the Universe and developing a detailed and coherent picture of how structure (galaxies, clusters of galaxies, superclusters, voids, great walls, and so on) developed. At present there is a working hypothesis—cold dark matter—which is based upon inflation and which, if correct, would extend the big bang model back to 10−32 sec and cast important light on the unification of the forces. Many experiments and observations, from CBR anisotropy experiments to Hubble Space Telescope observations to experiments at Fermilab and CERN, are now putting the cold dark matter theory to the test. At present it appears that the theory is viable only if the Hubble constant is smaller than current measurements indicate (around 30 km s−1 Mpc−1), or if the theory is modified slightly, e.g., by the addition of a cosmological constant, a small admixture of hot dark matter (5 eV “worth of neutrinos”), more relativistic particles, or a tilted spectrum of density perturbations.

Type
Part I: Invited Reviews
Information
Symposium - International Astronomical Union , Volume 168: Examining the Big Bang and the Diffuse Background Radiations , 1996 , pp. 301 - 320
Copyright
Copyright © Kluwer 1996 

References

[1] For textbooks on modern cosmology see e.g., Kolb, E.W. and Turner, M.S., The Early Universe (Addison-Wesley, Redwood City, CA, 1990) or Peebles, P.J.E., Principles of Physical Cosmology (Princeton University Press, Princeton, NJ, 1993).Google Scholar
[2] See e.g., Mould, J. et al., Astrophys. J. 383, 467 (1991).CrossRefGoogle Scholar
[3] Mather, J. et al., Astrophys. J. 420, 439 (1994).CrossRefGoogle Scholar
[4] See e.g., White, M., Scott, D., and Silk, J., Ann. Rev. Astron. Astrophys. 32, 319 (1994).CrossRefGoogle Scholar
[5] Copi, C., Schramm, D.N. and Turner, M.S., Science 267, 192 (1995).CrossRefGoogle Scholar
[6] See e.g., Efstathiou, G., in The Physics of the Early Universe, eds. Peacock, J.A., Heavens, A.F. and Davies, A.T. (Adam Higler, Bristol, 1992).Google Scholar
[7] See e.g., Weinberg, S., Gravitation and Cosmology (J. Wiley, New York, 1972).Google Scholar
[8] See e.g., Arp, H. et al., Nature 346, 807 (1990).CrossRefGoogle Scholar
[9] Jacoby, G.H. et al., Proc. Astron. Soc. Pacific 104, 599 (1992); Fukugita, M., Hogan, C.J., and Peebles, P.J.E., Nature 366, 309 (1993); Freedman, W. et al, Nature 371, 757 (1994).CrossRefGoogle Scholar
[10] Smoot, G. et al., Astrophys. J. 396, L1 (1992).CrossRefGoogle Scholar
[11] Ostriker, J.P., Ann. Rev. Astron. Astrophys. 31, 689 (1993).CrossRefGoogle Scholar
[12] Hoyle, F., Burbidge, G., and Narlikar, J.V., Astrophys. J. 410, 437 (1993); Mon. Not. R. astron. Soc. 267, 1007 (1994); Astron. Astrophys. 289, 729 (1994).CrossRefGoogle Scholar
[13] Faber, S. and Gallagher, J., Ann. Rev. Astron. Astrophys. 17, 135 (1979).CrossRefGoogle Scholar
[14] Trimble, V., Ann. Rev. Astron. Astrophys. 25, 425 (1987).CrossRefGoogle Scholar
[15] See e.g., Kaiser, N. et al., Mon. Not. R. astr. S. 252, 1 (1991); Strauss, M. A. et al., Astrophys. J. 397, 395 (1992); Dekel, A., Ann. Rev. Astron. Astrophys. 32, 371 (1994).CrossRefGoogle Scholar
[16] Peebles, P.J.E., Nature 327, 210 (1987); Astrophys. J. 315, L73 (1987).CrossRefGoogle Scholar
[17] Guth, A., Phys. Rev. D 23, 347 (1981).CrossRefGoogle Scholar
[18] Turner, M.S., Proc. Natl. Acad. Sci. (USA) 90, 4822 (1993).Google Scholar
[19] See e.g., Turok, N., Physica Scripta T36, 135 (1991).CrossRefGoogle Scholar
[20] Hu, W. and Sugiyama, N., astro-ph/9403031.Google Scholar
[21] Peebles, P.J.E., Astrophys. J. 432, L1 (1994).CrossRefGoogle Scholar
[22] See e.g., Linde, A.D., Particle Physics and Inflationary Cosmology (Harwood, Chur, 1990), or Turner, M. S., in Proceedings of TASI-92 , eds. Harvey, J. and Polchinski, J. (World Scientific, Singapore, 1993).Google Scholar
[23] Inflationary models have been constructed with Ω0 < 1; see e.g., Steinhardt, P. J., Nature 345, 47 (1990); Bucher, M. et al., hepth/9411206.CrossRefGoogle Scholar
[24] Guth, A. H. and Pi, S.-Y., Phys. Rev. Lett. 49, 1110 (1982); Hawking, S. W., Phys. Lett. B 115, 295 (1982); Starobinskii, A. A., ibid 117, 175 (1982); Bardeen, J. M., Steinhardt, P. J., and Turner, M. S., Phys. Rev. D 28, 697 (1983).CrossRefGoogle Scholar
[25] Rubakov, V.A., Sazhin, M., and Veryaskin, A., Phys. Lett. B 115, 189 (1982); Fabbri, R. and Pollock, M., ibid 125, 445 (1983); Starobinskii, A. A. Sov. Astron. Lett. 9, 302 (1983); Abbott, L. and Wise, M., Nucl. Phys. B 244, 541 (1984).CrossRefGoogle Scholar
[26] See e.g., Blumenthal, G.R. et al., Nature 311, 517 (1984).CrossRefGoogle Scholar
[27] Liddle, A.D. and Lyth, D., Phys. Repts. 231, 1 (1993).CrossRefGoogle Scholar
[28] Turner, M.S., Physica Scripta T36, 177 (1991).CrossRefGoogle Scholar
[29] Steinhardt, P.J. and Turner, M.S., Phys. Rev. D 29, 2162 (1984).CrossRefGoogle Scholar
[30] Kamionkowski, M. et al., Astrophys. J. 426, L57 (1994).CrossRefGoogle Scholar
[31] See e.g., Briel, U.G. et al., Astron. Astrophys. 259, L31 (1992); White, S.D.M. et al., Nature 366, 429 (1993); White, D. A. and Fabian, A. C., Mon. Not. R. astron. Soc., in press (1995).Google Scholar
[32] See e.g., Bahcall, J. et al., Astrophys. J. 435, L51 (1994) and References therein.CrossRefGoogle Scholar
[33] Gates, E., Gyuk, G., and Turner, M.S., astro-ph/9411073; Alcock, C. et al., astro-ph/9501091.Google Scholar
[34] Copeland, E.J., Kolb, E.W., Liddle, A.R., and Lidsey, J.E., Phys. Rev. Lett. 71, 219 (1993); Phys. Rev. D 48, 2529 (1993); Turner, M. S., ibid, 3502 (1993); Turner, M. S., ibid 48, 5539 (1993); Knox, L. and Turner, M. S., Phys. Rev. Lett. 73, 3347 (1994); Knox, L., Phys. Rev. D, in press (1995).CrossRefGoogle Scholar