scholarly journals Matter non-conservation in the universe and dynamical dark energy

2012 ◽  
Vol 29 (21) ◽  
pp. 215002 ◽  
Author(s):  
Harald Fritzsch ◽  
Joan Solà
2019 ◽  
Vol 28 (15) ◽  
pp. 1950167
Author(s):  
N. M. Jiménez Cruz ◽  
Celia Escamilla-Rivera

In this paper, we study the cosmological evolution of the universe filled with a perfect fluid in the Eddington-inspired-Born–Infeld gravity. Applying an alternative method in which the evolution of the scale factor for this theory is linked to the cosmographic parameters, we obtain a dynamical dark energy solution where the singularity (through a regular bounce or a loitering phase) still can be avoided for [Formula: see text] with [Formula: see text]. For the range [Formula: see text], the results lead us to universes that experience an unlimited rate of expansion with finite density. Also, we obtain a possible maximum value of [Formula: see text] at the cosmic bounce point.


2017 ◽  
Vol 26 (10) ◽  
pp. 1750115 ◽  
Author(s):  
Christine R. Farrugia ◽  
Joseph Sultana

As evidenced by a great number of works in the literature, it is common practice to assume that the universe is flat. However, the majority of studies which make use of observational data to constrain the curvature density parameter are premised on the [Formula: see text]CDM cosmology, or extensions thereof. On the other hand, when data is fitted to models with a time-varying dark energy equation-of-state, it turns out that such models may accommodate a non-flat universe. Several authors caution that if the assumption of spatial flatness is wrong, it could greatly hinder our understanding of dark energy, even if the curvature is in reality very small. We thus consider a number of different dynamical dark energy models that represent the complete cosmological scenario, and investigate the effects of spatial curvature on the evolution. We find that for a closed universe, the transition to the epoch of decelerated expansion would be delayed with respect to the flat case. So would the start of the current dark energy-dominated era. This would be accompanied by a larger inflationary acceleration, as well as a larger subsequent deceleration. The opposite behavior is observed if the universe is open.


2020 ◽  
Author(s):  
Jackie Liu

Abstract We develop a mechanism to generate dynamical dark energy - a quintessence field coupled with gravity. Such model causes the dark energy behaving differently in early and late time universe. In the radiation-dominated-era and matter-dominated-era, the related analytical solutions of the quintessence field have an interesting property - starting as a constant field, then oscillating as the universe expands. By Markov Chain Monte Carlo search of the parameter space with the local measurement (Type Ia supernovae) in the Bayesian framework, the probed range of H0 (within 1σ) overlaps the H0 value inferred from Planck CMB dataset by ΛCDM model.


2014 ◽  
Vol 29 (25) ◽  
pp. 1450119 ◽  
Author(s):  
Suresh Kumar

Chevallier–Polarski–Linder (CPL) parametrization for the equation of state (EoS) of dark energy in terms of cosmic redshift or scale factor have been frequently studied in the literature. In this study, we consider cosmic time-based CPL parametrization for the EoS parameter of the effective cosmic fluid that fills the fabric of spatially flat and homogeneous Robertson–Walker (RW) spacetime in General Relativity. The model exhibits two worthy features: (i) It fits the observational data from the latest H(z) and Union 2.1 SN Ia compilations matching the success of ΛCDM model. (ii) It describes the evolution of the Universe from the matter-dominated phase to the recent accelerating phase similar to the ΛCDM model but leads to Big Rip end of the Universe contrary to the everlasting de Sitter expansion in the ΛCDM model. We investigate the matter and dark energy sources in the model, in particular, behavior of the dynamical dark energy responsible for the Big Rip end of Universe.


Author(s):  
Nick E. Mavromatos ◽  
Joan Solà Peracaula

AbstractIn previous works, we have derived a Running Vacuum Model (RVM) for a string Universe, which provides an effective description of the evolution of 4-dimensional string-inspired cosmologies from inflation till the present epoch. In the context of this “stringy RVM” version, it is assumed that the early Universe is characterised by purely gravitational degrees of freedom, from the massless gravitational string multiplet, including the antisymmetric tensor field. The latter plays an important role, since its dual gives rise to a ‘stiff’ gravitational axion “matter”, which in turn couples to the gravitational anomaly terms, assumed to be non-trivial at early epochs. In the presence of primordial gravitational wave (GW) perturbations, such anomalous couplings lead to an RVM-like dynamical inflation, without external inflatons. We review here this framework and discuss potential scenarios for the generation of such primordial GW, among which the formation of unstable domain walls, which eventually collapse in a non-spherical-symmetric manner, giving rise to GW. We also remark that the same type of “stiff” axionic matter could provide, upon the generation of appropriate potentials during the post-inflationary eras, (part of) the Dark Matter (DM) in the Universe, which could well be ultralight, depending on the parameters of the string-inspired model. All in all, the new (stringy) mechanism for RVM inflation preserves the basic structure of the original (and more phenomenological) RVM, as well as its main advantages: namely, a mechanism for graceful exit and for generating a huge amount of entropy capable of explaining the horizon problem. It also predicts axionic DM and the existence of mild dynamical Dark Energy (DE) of quintessence type in the present universe, both being “living fossils” of the inflationary stages of the cosmic evolution. Altogether the modern RVM appears to be a theoretically sound (string-based) approach to cosmology with a variety of phenomenologically testable consequences.


2019 ◽  
Vol 64 (11) ◽  
pp. 998 ◽  
Author(s):  
B. Novosyadlyj

The properties and observational manifestations of the dynamical dark energy on the cosmological and astrophysical scales are discussed. We consider the dynamical dark energy in the form of quintessential and phantom scalar fields with different parameters of the equation of state and the effective sound speed. The evolution of the dynamical dark energy and its impact on the dynamics of expansion of the Universe, halos, and voids, and its behavior in the static gravitational fields of astrophysical objects are analyzed. The current state and possible tests designed to establish the nature of dark energy are highlighted.


Author(s):  
Manisha Banerjee ◽  
Sudipta Das ◽  
Abdulla Al Mamon ◽  
Subhajit Saha ◽  
Kazuharu Bamba

Recently, a novel equation of state (EoS) parameter for dark energy has been introduced which deals with a special mathematical function, known as the Lambert [Formula: see text] function. In this paper, we study the effect on the growth of perturbations for the Lambert [Formula: see text] dark energy model. We perform the analysis for two different approaches. In the first case, we consider the universe to be filled with two different fluid components, namely, the baryonic matter component and the Lambert [Formula: see text] dark energy component, while in the second case, we consider that there is a single fluid component in the universe whose equation of state parameter is described by the Lambert [Formula: see text] function. We then compare the growth rates of Lambert [Formula: see text] model with that for a standard [Formula: see text]CDM model as well as the CPL model. Our results indicate that the presence of Lambert [Formula: see text] dynamical dark energy sector changes the growth rate and affects the matter fluctuations in the universe to a great extent.


2021 ◽  
Vol 103 (2) ◽  
Author(s):  
Anton Chudaykin ◽  
Konstantin Dolgikh ◽  
Mikhail M. Ivanov

Author(s):  
Michael Kachelriess

The contribution of vacuum fluctuations to the cosmological constant is reconsidered studying the dependence on the used regularisation scheme. Then alternative explanations for the observed accelerated expansion of the universe in the present epoch are introduced which either modify gravity or add a new component of matter, dubbed dark energy. The chapter closes with some comments on attempts to quantise gravity.


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