Space-time dimension, Euclidean action and signature change

Abstract

This talk is devoted to the problem how to compute relative nucleation probabilities of configurations with different topology and dimension in quantum cosmology. Assuming the semiclassical approximation, the usual formula for the nucleation probability induced by the no-boundary wave function is $P_{NB}\approx\exp(-I)$, where $I$ is the Euclidean action, evaluated at a solution of the Euclidean Einstein equations with effective cosmological constant $\Lambda$. Relative probabilities of different configurations are usually compared at equal values of $\Lambda$. When configurations with different dimensions are admitted (the $n$-dimensional gravitational constant being subject to a rather mild restriction), as e.g. ${\bf S}^n$ for any $n$, this procedure leads to the prediction that the space-time dimension tends to be as large as possible. In this contribution, I would like to propose an alternative scheme, namely to compare the probabilities $P_{NB}\approx\exp(-I)$ at equal values of the {\it energy} $E$, instead of the {\it energy density} $\Lambda$. As a result, the space-time dimension settles at $n=4$. Attempts to predict the topology of the spacelike slices lead to the candidates ${\bf S}^3$ and ${\bf S}^1\times {\bf S}^2$. Since the ''process'' of nucleation (possibly connected with decoherence) is not well known in detail, we expect that either {\it both} configurations may be realized with roughly equal probability, or the {\it latter} one is favoured. Finally, we comment on the analogous situation based on the tunneling wave function.Comment: 11 pages, LaTeX, 3 Figures are available as hard copies; Talk given at the 3rd Alexander Friedmann international seminar on gravitation and cosmology; St. Petersburg, July 4 - 12, 199