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Andronikos Paliathanasis

Publications and source records attributed to Andronikos Paliathanasis.

At least 199 records · Page 11Linked to original sources
arXiv2020

Nonlinear interacting cosmological models after Planck 2018 legacy release and the $H_0$ tension

Interacting dark energy models are widely renowned for giving an explanation to the cosmic coincidence problem as well as several observational issues. According to the recent observational data, and so far we are concerned with the literature, the choice of the interaction function between dark matter and dark energy is always questionable since there is no such underlying theory that could derive it. Thus, in this work we have raised this issue by proposing two new nonlinear interaction functions and constrain them using cosmic microwave background (CMB) from Planck 2018, baryon acoustic oscillations (BAO), dark energy survey and a measurement of the Hubble constant $H_0$ from Hubble Space Telescope (HST) 2019. The dark energy equation of state is considered to be constant throughout the work and the geometry of the universe is assumed to be homogeneous and isotropic with zero spatial curvature. Our analyses report that a non-zero interaction is always allowed by the observational data and the dark energy equation of state is bent towards the phantom regime. In particular, when $H_0$ from HST is added to Planck 2018+BAO, we find an evidence for a non-zero coupling at more than $2σ$ confidence level. Our analyses also report that for both the models, $H_0$ is close to its local measurements and thus alleviating the $H_0$ tension. In particular, one of the interacting models perfectly solves the $H_0$ tension.

astro-ph.CO↗
arXiv2020

Dynamics and cosmological evolution in Λ-varying cosmology

We study the dynamical properties of a large body of varying vacuum cosmologies for which dark matter interacts with vacuum. In particular, performing the critical point analysis we investigate the existence and the stability of cosmological solutions which describe de-Sitter, radiation and matter dominated eras. We find several cases of varying vacuum models that admit stable critical points, hence they can be used in describing the cosmic history.

gr-qc↗
arXiv2020

Cosmological Evolution of Two-Scalar fields Cosmology in the Jordan frame

In the present article we study the cosmological evolution of a two-scalar field gravitational theory defined in the Jordan frame. Specifically, we assume one of the scalar fields to be minimally coupled to gravity, while the second field which is the Brans-Dicke scalar field is nonminimally coupled to gravity and also coupled to the other scalar field. In the Einstein frame this theory reduces to a two-scalar field theory where the two fields can interact only in the potential term, which means that the quintom theory is recovered. The cosmological evolution is studied by analyzing the equilibrium points of the field equations in the Jordan frame. We find that the theory can describe the cosmological evolution in large scales, while inflationary solutions are also provided.

gr-qc↗
arXiv2019

Similarity solutions for the Wheeler-DeWitt equation in $f\left( R\right) $-cosmology

In the case of a spatially flat Friedmann--Lema\^ıtre--Robertson--Walker universe in $f\left( R\right) $-gravity we write the Wheeler-DeWitt equation of quantum cosmology. The equation depends on the functional form of $f\left( R\right) $. We select to work with four specific functions of $f\left( R\right) $, in which the field equations for the classical models are integrable and solvable through quadratures. For these models, we determine similarity solutions for the Wheeler-DeWitt equation by determine Lie-Bäcklund transformations. In addition we show how the classical limit is recovered by the similarity solutions of the Wheeler-DeWitt equation.

gr-qc↗
arXiv2019

Challenging bulk viscous unified scenarios with cosmological observations

In a spatially flat Friedmann-Lemaître-Robertson-Walker universe, we investigate a unified cosmic fluid scenario endowed with bulk viscosity in which the coefficient of the bulk viscosity has a power law evolution. The power law in the bulk viscous coefficient is a general case in this study which naturally includes several choices as special cases. Considering such a general bulk viscous scenario, in the present work we have extracted the observational constraints using the latest cosmological datasets and examine their behaviour at the level of both background and perturbations. From the observational analyses, we find that a non-zero bulk viscous coefficient is always favored and some of the models in this series are able to weaken the current tension on $H_0$ for some dataset. However, from the Bayesian evidence analysis, $Λ$CDM is favored over the bulk viscous model.

astro-ph.CO↗
arXiv2019

Symmetry Analysis In Inflationary Cosmology

We approach the cosmological inflation thought symmetries of differential equations. We consider the general inflaton field in a homogeneous Friedmann--Lema\^ıtre--Robertson--Walker spacetime and with the use of conformal transformations we are able to write the generic algebraic solution for the field equations. We put emphasis on the inflationary models and we show how we can construct new inflationary models from already known models by using symmetry transformations.

gr-qc↗
arXiv2019

Reconstructing the dark matter and dark energy interaction scenarios from observations

We consider a class of interacting dark energy models in a flat and nonflat FLRW universe where the interaction is characterized by the modified evolution of the pressureless dark matter as $a^{-3+δ(a)}$, $a$ being the FLRW scale factor and $δ(a)$ quantifies the interaction rate. By assuming the most natural and nonsingular parametrization for $δ(a)$ as $δ\left( a\right) =\sum_{i} δ_i (1-a)^i $, where $δ_{i}$'s ($i=0,1,2,3,..$) are constants, we reconstruct the expansion history of the universe for three particular choices of the DE sector using different cosmological datasets. Our analyses show that the non-interacting scenario is consistent with the observations while the interaction is not strictly ruled out. We reconstruct in the following way. We start with the first two terms of $δ(a)$ above and constrain $δ_0$, $δ_1$. Then we consider up to the second order terms in $δ(a)$ but fix $δ_0$, $δ_1$ to their constrained values and constrain $δ_2$; similarly we constrain $δ_3$, and finally we constrain $(δ_0, δ_1, δ_1, δ_3)$ by keeping all of them to be free as a generalized case. Our reconstruction technique shows that the constraints on $δ_2$ (fixing $δ_0$ and $δ_1$) and $δ_3$ (fixing $δ_0$, $δ_1$ and $δ_2$) are almost zero for any interaction model and thus the effective scenario is well described by the linear parametrization $δ(a)\simeq δ_{0}+δ_{1}(1-a)$. Additionally, a strong negative correlation between $δ_0$, $δ_1$ is observed independently of the dark energy fluid and the curvature of our universe.

astro-ph.CO↗
arXiv2019

Observational constraints of a new unified dark fluid and the $H_0$ tension

Unified cosmological models have received a lot of attention in astrophysics community for explaining both the dark matter and dark energy evolution. The Chaplygin cosmologies, a well known name in this group have been investigated matched with observations from different sources. Obviously, Chaplygin cosmologies have to obey restrictions in order to be consistent with the observational data. As a consequence, alternative unified models, differing from Chaplygin model, are of special interest. In the present work we consider a specific example of such a unified cosmological model, that is quantified by only a single parameter $μ$, that can be considered as a minimal extension of the $Λ$-cold dark matter cosmology. We investigate its observational boundaries together with an analysis of the universe at large scale. Our study shows that at early time the model behaves like a dust, and as time evolves, it mimics a dark energy fluid depicting a clear transition from the early decelerating phase to the late cosmic accelerating phase. Finally, the model approaches the cosmological constant boundary in an asymptotic manner. We remark that for the present unified model, the estimations of $H_0$ are slightly higher than its local estimation and thus alleviating the $H_0$ tension.

gr-qc↗
arXiv2019

Similarity Inner Solutions for the Pulsar Equation

Lie symmetries are applied to classify the source of the magnetic field for the Pulsar equation near to the surface of the neutron star. We find that there are six possible different admitted Lie algebras. We apply the corresponding Lie invariants to reduce the Pulsar equation close to the surface to an ordinary differential equation. This equation is solved either with the use of Lie symmetries or the application of the ARS algorithm for singularity analysis to write the analytic solution as a Laurent expansion. These solutions are called inner solutions.

astro-ph.HE↗
arXiv2019

One-dimensional optimal system for 2D Rotating Ideal Gas

We derive the one-dimensional optimal system for a system of three partial differential equations which describe the two-dimensional rotating ideal gas with polytropic parameter $γ>2.$ The Lie symmetries and the one-dimensional optimal system are determined for the nonrotating and rotating systems. We compare the results and we found that when there is no Coriolis force the system admits eight Lie point symmetries, while the rotating system admits seven Lie point symmetries. Consequently the two systems are not algebraic equivalent as in the case of $γ=2~$ which was found by previous studies. For the one-dimensional optimal system we determine all the Lie invariants, while we demonstrate our results by reducing the system of partial differential equations into a system of first-order ordinary differential equations which can be solved by quadratures.

nlin.SI↗
arXiv2019

Static Spherically Symmetric Einstein-aether models II: Integrability and the Modified Tolman-Oppenheimer-Volkoff approach

We investigate the existence of analytic solutions for the field equations in the Einstein-æther theory for a static spherically symmetric spacetime and provide a detailed dynamical system analysis of the field equations. In particular, we investigate if the gravitational field equations in the Einstein-æther model in the static spherically symmetric spacetime possesses the Painlevè property, so that an analytic explicit integration can be performed. We find that analytic solutions can be presented in terms of Laurent expansion only when the matter source consists of a perfect fluid with linear equation of state (EoS) $μ=μ_{0}+\left( \texttt{h} -1\right) p,~\texttt{h} >1$. In order to study the field equations we apply the Tolman-Oppenheimer-Volkoff (TOV) approach and other approaches. We find that the relativistic TOV equations are drastically modified in Einstein-æther theory, and we explore the physical implications of this modification. We study perfect fluid models with a scalar field with an exponential potential. We discuss all of the equilibrium points and discuss their physical properties.

gr-qc↗
arXiv2019

Extended phase-space analysis of the Horava-Lifshitz cosmology

We examine the phase space of Hořava-Lifshitz cosmology for a wide range of self-interacting potentials for the scalar field under the detailed-balance condition and without imposing it, by means of the powerful method of $f$-devisers. A compactification approach is performed for the exponential potential and for potentials beyond the exponential one, extending the previous findings in the literature. By using this approach it is possible to describe the finite region of the phase space and the region where the phase-space variables becomes infinity. Furthermore, we present several results concerning the stability of the \emph{de Sitter} solution in Hořava-Lifshitz cosmology using Center Manifold theory. The advantages of this procedure are unveiled immediately when it is compared with the Normal Forms Calculations presented before in the literature.

gr-qc↗
arXiv2019

Exact Solutions in Chiral Cosmology

In multi-scalar field cosmologies new dynamical degrees of freedom are introduced which can explain the observational phenomena. Unlike the usual scalar field theory where a single scalar field is considered, the multi-scalar field cosmologies allow more than one scalar field and exhibits interetsing consequences, such as quintom, hybrid inflation etc. The current work studies the existence of exact solutions and integrable dynamical systems in multi-scalar field cosmology. We present the exact analytic solutions for a system of $N$-scalar fields. In particular, we consider a multi scalar field cosmological scenario comprised of $N$-scalar fields that are minimally coupled to the Einstein gravity. The geometry of the universe is described by the spatially flat homogeneous and isotropic line element and the scalar fields may interact in their kinetic or/and potential terms. Within this set up, we show that for a specific geometry in the kinetic part of the scalar fields and specific potential form, the gravitational field equations for the class of $N$-scalar field models can be exactly solved. More specifically, we show that the Einstein field equations in $N$-scalar field cosmology can be reduced to that of a $\left( N+1\right) $ linear system.

gr-qc↗
arXiv2019

Dynamics of Einstein-Aether Scalar field Cosmology

We study the cosmological evolution of the field equations in the context of Einstein-Aether cosmology by including a scalar field in a spatially flat Friedmann--Lema\^ıtre--Robertson--Walker spacetime. Our analysis is separated into two separate where a pressureless fluid source is included or absent. In particular, we determine the critical points of the field equations and we study the stability of the specific solutions. The limit of general relativity is fully recovered, while the dynamical system admits de Sitter solutions which can describe the past inflationary era and the future late-time attractor. Results for generic scalar field potentials are presented while some numerical behaviours are given for specific potential forms.

gr-qc↗
arXiv2019

A Systematic Analysis of the Properties of the Generalised Painlevé--Ince Equation

We consider the generalized Painlevé--Ince equation, \begin{equation*} \ddot{x}+αx\dot{x}+βx^{3}=0 \end{equation*} and we perform a detailed study in terms of symmetry analysis and of the singularity analysis. When the free parameters are related as $β=α^{2}/9~$the given differential equation is maximally symmetric and well-known that it pass the Painlevé test. For arbitrary parameters we find that there exists only two Lie point symmetries which can be used to reduce the differential equation into an algebraic equation. However, the generalized Painlevé--Ince equation fails at the Painlevé test, except if we apply the singularity analysis for the new second-order differential equation which follows from the change of variable $x=1/y.$ We conclude that the Painlevé--Ince equation is integrable is terms of Lie symmetries and of the Painlevé test.

nlin.SI↗
arXiv2019

Conservation laws and Exact Solutions in Brans-Dicke Cosmology with a Scalar Field

Scalar-tensor theories have drawn the attention of cosmologist for the past few years because they can provide mechanism to explain the observable phenomena. Moreover, the results of scalar-tensor theories can be applied in higher-order theories of gravity. In this work, we consider a Brans-Dicke scalar field cosmological model that includes a second scalar field minimally coupled to gravity. For the second scalar field we consider the two cases that there exist and there is not any interaction with the Brans-Dicke scalar field. For the two models of our consideration we prove the existence of scaling and de Sitter solutions. Furthermore, we perform an Obsiannikov's classification for the field equations, where we find all the point and contact transformations which leave the gravitational Action Integral invariant. Conservation laws are determined and we show how these can be applied to infer about the integrability of the cosmological models and find new analytic solutions.

gr-qc↗
arXiv2019

Constructing the CKVs of Bianchi III and V spacetimes

We determine the conformal algebra of Bianchi III and Bianchi V spacetimes or, equivalently, we determine all Bianchi III and Bianchi V spacetimes which admit a proper conformal Killing vector. The algorithm that we use has been developed in Class. Quantum. Grav. 15, 2909 (1998) and concerns the computation of the CKVs of decomposable spacetimes. The main point of this method is that a decomposable space admits a CKV if the reduced space admits a gradient homothetic vector the latter being possible only if the reduced space is flat or a space of constant curvature. We apply this method in a stepwise manner starting from the two dimensional spacetime which admits an infinite number of CKVs and we construct step by step the Bianchi III and V spacetimes by assuming that CKVs survive as we increase the dimension of the space. We find that there is only one Bianchi III and one Bianchi V spacetime which admit at maximum one proper CKV. In each case we determine the conformal Killing vector and the corresponding conformal factor. As an application in the spacetimes we found we study the kinematics of the comoving observers and the dynamics of the corresponding cosmological fluid. As a second application we determine in these spacetimes generators of the Lie symmetries of the wave equation.

gr-qc↗