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By Peter G. Bergmann (auth.), Peter C. Aichelburg, Roman U. Sexl (eds.)

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Nat. Acad. Sci. S. 15, p. 169, (1929). [6] E. P. Hubble, 'The Realm of the Nebulae", New Haven, Yale Univ. Press, 1936. (7] H. P. Robertson, "Kinematics and world structure", Astrophys. J. 82, p. 248, (1935). [8] A. G. Walker, "On Riemannian spaces with spherical symmetry about a line and isotropy in general relativity", J. Math. Oxford Ser. 6, 81 (1935). [9] A. Einstein, W. de Sitter, "On the relation between the expansion of the universe", Proc. Nat. Acad. Sci. 18,213 (1932). [10] H. Bondi und T.

10] H. Bondi und T. Gold, "The steady-state theory of the expanding universe", Mon. Not. R. Astron. Soc. 108, p. 252 (1948). [11] F. Hoyle, "A new model for the expanding universe", Mon. Not. R. Astron. Soc. 108, p. 372, (1948) [12] A. A. Penzias und R. W. s", Astrophys. J 142, p. 419 (1965). [13] R. H. ]. Peebles, P. G. Roll und D. T. Wilkinson, "Cosmic-black-body radiation", Astrophys. J. 142, p. 414 (1965). [14] G. Gamow. "The evolution of the universe", Nature 162, p. 680, (1948). [15] R. A.

18 Dennis W. Sciama The second idea was by no means obvious, and this was to exploit the non-Euclidean geometry of his theory by constructing a model in which space at anyone time is finite but unbounded - the three-dimensional analogue of the surface of a sphere. The topology of space as well as its geometry was thus brought into the discussion. The next major step was taken in 1922 by a Russian meteorologist Alexander Friedmann [3]. He showed that by not insisting that the universe be static one could construct a whole family of homogeneous and isotropic models, with or without the cosmological term.

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