Hostname: page-component-586b7cd67f-t7fkt Total loading time: 0 Render date: 2024-11-30T00:37:17.375Z Has data issue: false hasContentIssue false
  • English
  • Français

Self-Similar Gravitational Clustering

Published online by Cambridge University Press:  04 August 2017

G. Efstathiou
G. Efstathiou*
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge, England

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The nature of the distribution of galaxies poses a challenging problem for theorists. It seems reasonable, as a start, to suppose that galaxies and clusters arose from small perturbations by gravitational instability. However, one still has the problem of the choice of initial conditions, for example, the shape of the fluctuation spectrum and the cosmological density parameter Ω. A considerable simplification is to assume that the clustering pattern obeys some simple similarity scaling, so that the clustering at some early time, apart from a change in length scale, is statistically indistinguishable from the pattern observed today. The power-law shape of the two-point correlation function and the simple forms of higher order correlation functions (Peebles, 1980) have provided some evidence that such a simplifying assumption may be relevant - just how relevant is the subject of this article.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 104: Early Evolution of the Universe and Its Present Structure , 1983 , pp. 393 - 400
Copyright
Copyright © Reidel 1983 

References

Bean, J., Efstathiou, G., Ellis, R.S., Peterson, B.A. and Shanks, T.: 1982, in preparation.Google Scholar
Bond, J.R., Efstathiou, G. and Silk, J.: 1980, Phys. Rev. Lett., 45, 1180.Google Scholar
Bond, J.R., Szalay, A.S. and Turner, M.: 1982, Phys. Rev. Lett., 48, 1636.Google Scholar
Davis, M. and Peebles, P.J.E.: 1977, Ap.J. Suppl., 34, 425.CrossRefGoogle Scholar
Davis, M. and Peebles, P.J.E.: 1982, preprint.Google Scholar
Efstathiou, G. and Eastwood, J.W.: 1981, M.N.R.A.S., 194, 503.Google Scholar
Efstathiou, G., Fall, S.M. and Hogan, C.: 1979, M.N.R.A.S., 189, 203.Google Scholar
Frenk, C.S., White, S.D.M. and Davis, M.: 1982, preprint.Google Scholar
Fry, J.N. and Peebles, P.J.E.: 1980, Ap.J., 236, 13.Google Scholar
Gott, J.R., Turner, E.L. and Aarseth, S.J.: 1979, Ap.J., 234, 13.Google Scholar
Hogan, C. and Kaiser, N.: 1982, in preparation.Google Scholar
Kirshner, R.P., Oemler, A. and Schechter, P.L.: 1978, A.J., 83, 1549.Google Scholar
Klypin, A.A. and Shandarin, S.F.: 1982, preprint and this volume.Google Scholar
Miyoshi, K. and Kihara, T.: 1975, Pub. Astr. Soc. Japan, 27, 333 Google Scholar
Peebles, P.J.E.: 1976, Ap. J. Lett., 205, L109.Google Scholar
Peebles, P.J.E.: 1979, A.J., 84, 730.Google Scholar
Peebles, P.J.E.: 1980, “The Large-Scale Structure of the Universe”, Princeton University Press, Princeton, N.J. Google Scholar
Peebles, P.J.E.: 1982, preprint.Google Scholar
Peterson, B.A., Bean, J., Efstathiou, S., Ellis, R.S., Shanks, T. and Zou, , 1982, in preparation.Google Scholar
Soneira, R.M. and Peebles, P.J.E.: 1978, A.J., 83, 845.Google Scholar