Abstract
A recent work proposed that the recent cosmic passage to a cosmic acceleration era is the result of the existence of small anti-gravity sources in each galaxy and clusters of galaxies. In particular, a Swiss-cheese cosmology model, which relativistically integrates the contribution of all these anti-gravity sources on a galactic scale has been constructed assuming the presence of an infrared fixed point for a scale dependent cosmological constant. The derived cosmological expansion provides an explanation for both the fine tuning and the coincidence problem. The present work relaxes the previous assumption on the running of the cosmological constant and allows for a generic scaling around the infrared fixed point. Our analysis reveals that, in order to produce a cosmic evolution consistent with the best ΛCDM model, the IR-running of the cosmological constant is consistent with the presence of an IR-fixed point.
Highlights
The cosmological constant problem of quantum field theory, first emphasized by Zeldovich, is one of the greatest problems of modern theoretical physics
We chose the values of the free parameters as follows: One can choose any value of order one for ξ and γ, and b must have a value that ensures that the second term and the third term of Equation (11) are almost equal
A spatially homogeneous isotropic universe is filled with a large number of quantum improved Schwarzschild–de-Sitter black holes that are uniformly distributed throughout the space
Summary
The cosmological constant problem of quantum field theory, first emphasized by Zeldovich, is one of the greatest problems of modern theoretical physics. All homogeneously distributed anti-gravity sources from every galaxy or cluster of galaxies, we obtain a net effect on the cosmic expansion This “sum” can be performed adapting a Swiss-cheese model in which matching between the local and the cosmic patches generates the observed recent passage from deceleration to acceleration. K should be considered not as a momentum flowing into a loop, but as an inverse of a typical distance over which the averaging of the field variables is performed From this point of view, several works have discussed the possibility of interpreting astrophysical data as an infrared effect of quantum gravity, relating k to a cosmic time [36], or cosmic distance. We write b ≡ 2 − η, and b has to be determined by assuming an underling best-fit ΛCDM cosmology
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