arXiv subjects
Publications and source records attributed to H. V. Fagundes.
The cosmic crystallography method of Lehoucq et al. [1] produces sharp peaks in the distribution of distances between the images of cosmic sources. But the method cannot be applied to universes with compact spatial sections of negative curvature. We apply to these a second order crystallographic effect, as evidenced by statistical parameters.
We generalize a previously obtained result, for the case of a few other static hyperbolic universes with manifolds of nontrivial topology as spatial sections.
We clarify and develop the results of a previous paper on the birth of a closed universe of negative spatial curvature and multiply connected topology. In particular we discuss the initial instanton and the second topology change in more detail. This is followed by a short discussion of the results.
We try to apply the cosmic crystallography method of Lehoucq, Lachieze-Rey, and Luminet to a universe model with closed spatial section of negative curvature. But the sharp peaks predicted for Einstein-de Sitter closed models do not appear in our hyperbolic example. So we turn to a variant of that method, by subtracting from the distribution of distances between images in the closed model, the similar distribution in Friedmann's open model. The result is a plot with much oscillation in small scales, modulated by a long wavelength quasi-sinusoidal pattern.
We propose a modified form of the spontaneous birth of the universe by quantum tunneling. It proceeds through topology change and inflation, to eventually become a universe with closed spatial sections of negative curvature and nontrivial global topology.
A numerical integration is made, starting with a Kantowski-Sachs (KS) model with an added initial perturbation at time one-tenth the age of the universe, and evolving up to the present. According to a prediction by Barrow (1989), the ratio between the fluctuations of the average matter density and those of the metric tensor varies with the inverse squared wavelength of the fluctuation. In this paper we take an extravantly large value for this wavelength (20% of the horizon's radius), to see that even then that ratio remains greater than unity. So we may be reasonably confident of models assuming density homogeneity, despite the fact that the scale of observed structure in the universe has been increasing lately.