Abstract
The background cosmological dynamics of the late Universe is analysed on the framework of a dark energy model described by an holographic Ricci dark energy component. Several kind of interactions between the dark energy and the dark matter components are considered herein. We solve the background cosmological dynamics for the different choices of interactions with the aim to analyse not only the current evolution of the universe but also its asymptotic behaviour and, in particular, possible future singularities removal. We show that in most of the cases, the Big Rip singularity, a finger print of this model in absence of an interaction between the dark sectors, is substituted by a de Sitter or a Minkowski state. Most importantly, we found two new future bouncing solutions leading to two possible asymptotic behaviours, we named Little Bang and Little Sibling of the Big Bang. At a Little Bang, as the size of the universe shrinks to zero in an infinite cosmic time, the Hubble rate and its cosmic time derivative blow up. In addition, at a Little sibling of the Big Bang, as the size of the universe shrinks to zero in an infinite cosmic time, the Hubble rate blows up but its cosmic time derivative is finite. These two abrupt events can happen as well in the past.
Highlights
There are many dynamical models trying to explain the nature of Dark energy (DE) [5,6]
The background cosmological dynamics of the late Universe is analysed on the framework of a dark energy model described by an holographic Ricci dark energy component
We found two new future bouncing solutions leading to two possible asymptotic behaviours, we named Little Bang and Little Sibling of the Big Bang
Summary
There are many dynamical models trying to explain the nature of DE [5,6]. Among them, there is an attractive model which is inspired on the holographic principle rooted on quantum gravity [7,8,9]; it is the so called holographic dark energy [10,11]. When the inequality is saturated, we can define an energy density which is inversely proportional to the square of the characteristic length of the system These ideas have been applied to the universe giving rise to what is known as the holographic dark energy scenario [10]. An interaction on the dark sector and within the HRDE model has been previously analysed in [19,20,21,30,34,35,36] where the main goal of these papers was to study the adequacy (from an observational point of view) of these models to describe the late time acceleration rather than analysing the asymptotic behaviour of the universe.
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