arXiv subjects

D. L. Canedo

Publications and source records attributed to D. L. Canedo.

4 recordsLinked to original sources

arXiv2026

Resonances in the early Universe

In the present paper, we study a Friedmann-Lemaître-Robertson-Walker (FLRW) quantum cosmology model with positively curved spatial sections. The matter content of the model is given by a radiation fluid, a constant vacuum energy, and an ad hoc potential. After writing the Hamiltonian of the model, we notice that the effective potential ($V_{eff}$) depends on two parameters: $ρ_v$, the constant vacuum energy density and $σ$, associated with the ad hoc potential. Depending on the values of these parameters $V_{eff}$ becomes a double barrier potential. We quantize the model and obtain the Wheeler-DeWitt equation. We solve that equation using the WKB approximation and compute the corresponding probability ($TP_{WKB}$) that the wavefunction of the universe tunnels through the double barrier potential $V_{eff}$. We study how $TP_{WKB}$ behaves as a function of the parameters $ρ_v$, $σ$ and the radiation energy $E$. We notice the occurrence of resonances in $TP_{WKB}$ when we vary it as a function of $E$, $ρ_v$ and $σ$. It is a very interesting phenomenon because it may cause the universe to be born with selected values of $E$, $ρ_v$ and $σ$.

gr-qc↗

arXiv2025

Quantum Creation of a FRW Universe: applying the Riesz fractional derivative

In this work, we apply fractional calculus to study quantum cosmology. Specifically, our Wheeler-DeWitt equation includes a FRW geometry, a radiation fluid, a positive cosmological constant, and an ad hoc potential; we employ the Riesz fractional derivative, which brings a parameter $α$, where $1 < α\leq 2$, appearing explicitly in the mentioned equation. We investigate numerically the tunnelling probability for the Universe to emerge using a suitable WKB approximation. Our findings are as follows. When we decrease the value for $α$, the tunnelling probability also decreases, suggesting that if fractional features could be considered to ascertain among different early universe scenarios, then the value $α=2$ (meaning strict locality and standard cosmology) would be the most likely. Finally, our results also allow for an interesting discussion between selecting values for $Λ$ (in a non-fractional conventional set-up) versus balancing, e.g., both $Λ$ and $α$ in the fractional framework. Concretely, the probability transition in the former if, e.g., $Λ=0.7$, is very close to the value computed if in the latter we employ instead, e.g., $Λ=1.5$ and $α=1.9397961$.

gr-qc↗

arXiv2023

Tunneling probability for the birth of universes with radiation, cosmological constant and an ad hoc potential

In this work we study the birth of Friedmann-Lema\^ıtre-Robertson-Walker (FLRW) models with zero ($k=0$) and negative ($k=-1$) curvatures of the spatial sections. The material content of the models is composed of a radiation perfect fluid and a positive cosmological constant. The models also have the presence of an ad hoc potential which origin is believed to be of geometrical nature. In order to describe the birth of these universes, we quantize them using quantum cosmology. Initially, we obtain the Wheeler-DeWitt equations and solve them using the WKB approximation. We notice that the presence of the ad hoc potential produces a barrier for any value of $k$. It means that we may describe the birth of the universe through a tunneling mechanism, for any curvature of the spatial sections, not only for the usual case $k=1$. We, explicitly, compute the tunneling probabilities for the birth of the different models of the universe and compare these tunneling probabilities.

gr-qc↗

arXiv2021

An anisotropic Kantowski-Sachs universe with radiation, dust and a phantom fluid

In the present work, we study the dynamical evolution of an homogeneous and anisotropic KS cosmological model, considering general relativity as the gravitational theory, such that there are three different perfect fluids in the matter sector. They are radiation, dust and phantom fluid. Our main motivation is determining if the present model tends to an homogeneous and isotropic FRW model, during its evolution. Also, we want to establish how the parameters and initial conditions of the model, quantitatively, influence the isotropization of the present model. In order to simplify our task, we use the Misner parametrization of the KS metric. In terms of that parametrization the KS metric has two metric functions: the scale factor $a(t)$ and $β(t)$, which measures the spatial anisotropy of the model. We solve, numerically, the Einstein's equations of the model and find a solution where the universe starts to expand from a, small, initial size and continues to expand until it ends in a {\it Big Rip} singularity. We explicitly show that for the expansive solution, after same time, the universe becomes isotropic. Based on that result, we can speculate that the expansive solution may represent an initial, anisotropic, stage of our Universe, that later, due to the expansion, became isotropic.

gr-qc↗