Abstract
The importance of investigating particle horizons in order to interpret a cosmological solution of Einstein’s field equations has been described. We have presented the formula and studied the particle horizons in some of the cosmological models presented in our earlier papers. It is well known that the Friedman-Robertson-Walker (F-R-W) models, the energy density of the free gravitational field denoted by ε, equivalently denoted by MacCallum parameter ξ, vanishes but the particle horizons exist and thus the former has no bearing on the latter. However, we have shown in our models presented herein that ε is related with particle horizons. Further, it is shown that as ε grows, the segment of the corresponding particle horizon decreases and thus the radius of the corresponding visible universe decreases.
Highlights
Cosmology deals with the large scale structure of the universe, which by definition contains everything, viz., both observable and non observable
We have presented the formula and studied the particle horizons in some of the cosmological models presented in our earlier papers
It is well known that the Friedman-Robertson-Walker (F-R-W) models, the energy density of the free gravitational field denoted by ε, equivalently denoted by MacCallum parameter ξ, vanishes but the particle horizons exist and the former has no bearing on the latter
Summary
Cosmology deals with the large scale structure of the universe, which by definition contains everything, viz., both observable and non observable. Cosmological models with inhomogeneous density have been studied [1,2,3] It has been shown [4,5,6,7], that the energy density of the free gravitational field ε is related to both anisotropy and in homogeneity. In order to interpret a cosmological solution of Einstein’s field equations, one should investigate some special aspects like horizons [13,14]. It has been studied event horizons in cosmology [15].
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