Advertisement

The Simplest Picture of Galaxy Formation and Why It Fails

  • Malcolm S. Longair
Part of the Astronomy and Astrophysics Library book series (AAL)

Abstract

We are now in a position to make a first attempt at understanding how galaxies and the large-scale structure of the Universe came about. In this chapter, we examine the case in which it is assumed that all the matter in the Universe, both ‘visible’ and dark, is in baryonic form. This was the natural starting point for the first plausible models for galaxy formation in the 1960s and 1970s, but they are doomed to failure. Despite this, there are two good reasons for studying this case carefully. The first is that many important physical processes will be introduced which will be needed in the construction of acceptable models. The second aspect is that the failure of these models strongly suggests that the dominant dark matter present in the Universe must be in some non-baryonic form. We need to convince ourselves of the reasoning behind this dramatic conclusion — the nature of the non-baryonic dark matter is of fundamental importance for physics and cosmology.

Keywords

Sound Speed Cosmic Background Radiation Galaxy Formation Baryonic Mass Radiation Energy Density 
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.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

Reference

  1. Coles, P. and Lucchin, F. (1995). Cosmology — the Origin and Evolution of Cosmic Structure. Chichester: John Wiley and Sons.MATHGoogle Scholar
  2. Efstathiou, G. (1990). In Physics of the Early Universe, (eds. J.A. Peacock, A.F. Heavens & A.T. Davies), 361. Edinburgh: SUSSP Publications.Google Scholar
  3. Guth, A. (1981). Phys. Rev., D23, 347.ADSGoogle Scholar
  4. Padmanabhan, T. (1993). Structure Formation in the Universe. Cambridge: Cam-bridge University Press.Google Scholar
  5. Peebles, P.J.E. (1980). The Large-Scale Structure of the Universe. Princeton: Princeton University Press.Google Scholar
  6. Peebles, P.J.E. (1981). ApJ, 248, 885.ADSCrossRefGoogle Scholar
  7. Peebles, P.J.E. (1993). Principles of Physical Cosmology. Princeton: Princeton Uni-versity Press.Google Scholar
  8. Rindler, W. (1956). MNRAS, 116, 662.MathSciNetADSGoogle Scholar
  9. Sakharov, A.A. (1965). ZhETP, 49, 345. [English translation: (1966) Sov. Phys. JETP, 22, 241.]Google Scholar
  10. Silk, J. (1968). ApJ, 151, 459.ADSCrossRefGoogle Scholar
  11. Sunyaev, R.A. and Zeldovich, Ya.B. (1970). Ap. Sp. Sc, 7(1), 1.ADSGoogle Scholar
  12. Sunyaev, R.A. and Zeldovich, Ya.B. (1972). A&A, 20(2), 189.ADSGoogle Scholar
  13. Weinberg, S. (1972). Gravitation and Cosmology. New York: John Wiley and Co.Google Scholar
  14. Zeldovich, Ya.B. (1970). A&A, 5, 84.ADSGoogle Scholar
  15. Zeldovich, Ya.B. (1993). In Selected Works of Yakov Borisevich Zeldovich, Vol. 2. Particles, Nuclei and the Universe (eds. J.P. Ostriker, G.I. Barenblatt and R.A. Sunyaev). Princeton: Princeton University Press.Google Scholar

Copyright information

© Springer-Verlag Berlin Heidelberg 1998

Authors and Affiliations

  • Malcolm S. Longair
    • 1
  1. 1.Department of Physics, Cavendish LaboratoryUniversity of CambridgeCambridgeUK

Personalised recommendations