Annu. Rev. Astron. Astrophys. 1994. 32:
319-70
Copyright © 1994 by . All rights reserved |

**7.4. Topology**

The fluctuations at large angular scales can also be used to constrain
the topology of the Universe, which in principle could be nontrivial
(Zel'dovich 1973,
Sokolov & Starobinskii
1976,
Fang & Houjun 1987,
Fang 1991).
The Sachs-Wolfe spectrum of
*C*_{}s is an
integral over the
power spectrum (Equation 14) in an ordinary simply-connected universe,
but becomes a sum over modes that are harmonics of the box-size in a
universe that has the topology of a three-torus (i.e. has periodic
boundary conditions). This sum fails to accurately approximate the
integral on scales approaching that of the box. Then the fact that
*COBE* measures a roughly flat power spectrum on large scales means
that
the box must be roughly the horizon size or bigger, unless the initial
power spectrum has a pathological increase for small multipoles. More
detailed comparisons indicate that the scale of any such topology is
80% of the horizon size
(Stevens et al 1993,
Sokolov 1993,
Starobinskii 1993).

For open universes, Gurzadyan and collaborators have argued that
curvature effects may result in elongated shapes of anisotropies in
the CMB
(Gurzadyan & Kocharyan
1993,
Gurzadyan & Torres
1993).
The isotropy pattern of the CBR can also be used to place limits on the
rotation of the Universe
(Collins & Hawking
1973,
Barrow et al 1985).
Currently the limit on the dimensionless rotation is
/ *H*_{0}
10^{-6}
(Smoot 1992),
which is about 1" every 30 Gyr!