Dynamic minimally interacting holographic dark energy cosmological model in f(T) gravity

2018 ◽  
Vol 92 (11) ◽  
pp. 1485-1494 ◽  
Author(s):  
V. R. Chirde ◽  
S. H. Shekh
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Holographic Dark Energy

scholarly journals Cosmological evolution with interaction between dark energy and dark matter

2015 ◽  
Vol 24 (03) ◽  
pp. 1530007 ◽  
Author(s):  
Yuri L. Bolotin ◽  
Alexander Kostenko ◽  
Oleg A. Lemets ◽  
Danylo A. Yerokhin
Keyword(s):  
Dark Matter ◽  
Dark Energy ◽  
Cosmological Model ◽  
Holographic Dark Energy ◽  
Main Task ◽  
Nonlinear Interactions ◽  
Dark Sector ◽  
Standard Cosmological Model ◽  
Linear And Nonlinear ◽  
The Universe

In this review we consider in detail different theoretical topics associated with interaction in the dark sector. We study linear and nonlinear interactions which depend on the dark matter and dark energy densities. We consider a number of different models (including the holographic dark energy and dark energy in a fractal universe), with interacting dark energy and dark matter, have done a thorough analysis of these models. The main task of this review was not only to give an idea about the modern set of different models of dark energy, but to show how much can be diverse dynamics of the universe in these models. We find that the dynamics of a universe that contains interaction in the dark sector can differ significantly from the Standard Cosmological Model.

scholarly journals Holographic Dark Energy Cosmological Model in Scalar Tensor Theory of Gravitation

2017 ◽  
Vol 1 (2) ◽  
Author(s):  
V.G. Mete ◽  
◽  
V.D. Elkar ◽  
Poonam P. Kadu ◽  
◽  
...  
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Holographic Dark Energy ◽  
Scalar Tensor Theory ◽  
Tensor Theory ◽  
Theory Of Gravitation

Holographic dark energy model with quintessence in general class of Bianchi cosmological models

2015 ◽  
Vol 93 (1) ◽  
pp. 68-79
Author(s):  
R. Chaubey ◽  
A.K. Shukla
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
General Class ◽  
Holographic Dark Energy ◽  
Scale Factor ◽  
Cosmological Models ◽  
Negative Slope ◽  
Physical Parameters ◽  
Field Equations ◽  
Dark Energy Component

In this paper, we study the general class of Bianchi cosmological models with holographic dark energy component. We have discussed three types of solutions of the average scale factor for the general class of Bianchi cosmological models by using a special law for the deceleration parameter, which is linear in time with a negative slope. The exact solutions to the corresponding field equations are also obtained. All the physical parameters are calculated and discussed in each physically viable cosmological model. For large time (i.e., t → ∞) the models tend asymptotically to an isotropic Friedmann–Robertson–Walker cosmological model. Quintessence scalar field and quintessence potential are also obtained for three different scenarios of scale factor.

scholarly journals THE COSMOLOGICAL DYNAMICS OF INTERACTING HOLOGRAPHIC DARK ENERGY MODEL

2009 ◽  
Vol 18 (01) ◽  
pp. 147-157 ◽  
Author(s):  
M. R. SETARE ◽  
ELIAS C. VAGENAS
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Critical Points ◽  
Dark Energy Model ◽  
Holographic Dark Energy ◽  
Cosmic Acceleration ◽  
Holographic Dark Energy Model ◽  
Evolution Of The Universe ◽  
Energy Scenario ◽  
The Universe

Motivated by the recent observations for cosmic acceleration and the suitable evolution of the universe provided an interaction (decay of dark energy to matter) is incorporated in a cosmological model, we study the cosmological evolution of the interacting holographic dark energy scenario. Critical points are derived and their corresponding cosmological models are presented. The dynamical character of these models is revealed.

scholarly journals Logarithmic entropy corrected holographic dark energy with nonminimal kinetic coupling

2012 ◽  
Vol 90 (1) ◽  
pp. 61-66 ◽  
Author(s):  
Ali R. Amani ◽  
J. Sadeghi ◽  
H. Farajollahi ◽  
M. Pourali
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Dark Energy Model ◽  
Holographic Dark Energy ◽  
Energy Model ◽  
Kinetic Coupling ◽  
Phantom Dark Energy ◽  
Coupling Terms ◽  
Friedmann Robertson Walker

In this study, we have considered a cosmological model with nonminimal kinetic coupling terms and investigated its cosmological implications with respect to logarithmic entropy corrected holographic dark energy (LECHDE). The correspondence between LECHDE in flat Friedmann–Robertson–Walker cosmology and the phantom dark energy model is also examined with the aim of interpreting the current universe acceleration.

scholarly journals Cosmology in the mimetic higher-curvature $$f(R,R_{\mu \nu }R^{\mu \nu })$$ gravity

2021 ◽  
Vol 11 (1) ◽  
Author(s):  
Adam Z. Kaczmarek ◽  
Dominik Szczȩśniak
Keyword(s):  
Dark Energy ◽  
Energy Density ◽  
Cosmological Model ◽  
Holographic Dark Energy ◽  
Scalar Potential ◽  
De Sitter ◽  
Field Equations ◽  
Dark Energy Density ◽  
Planck Data ◽  
Reconstruction Scheme

AbstractIn the framework of the mimetic approach, we study the $$f(R,R_{\mu \nu }R^{\mu \nu })$$ f ( R , R μ ν R μ ν ) gravity with the Lagrange multiplier constraint and the scalar potential. We introduce field equations for the discussed theory and overview their properties. By using the general reconstruction scheme we obtain the power law cosmology model for the $$f(R,R_{\mu \nu }R^{\mu \nu })=R+d(R_{\mu \nu }R^{\mu \nu })^p$$ f ( R , R μ ν R μ ν ) = R + d ( R μ ν R μ ν ) p case as well as the model that describes symmetric bounce. Moreover, we reconstruct model, unifying both matter dominated and accelerated phases, where ordinary matter is neglected. Using inverted reconstruction scheme we recover specific $$f(R,R_{\mu \nu }R^{\mu \nu })$$ f ( R , R μ ν R μ ν ) function which give rise to the de-Sitter evolution. Finally, by employing the perfect fluid approach, we demonstrate that this model can realize inflation consistent with the bounds coming from the BICEP2/Keck array and the Planck data. We also discuss the holographic dark energy density in terms of the presented $$f(R,R_{\mu \nu }R^{\mu \nu })$$ f ( R , R μ ν R μ ν ) theory. Thus, it is suggested that the introduced extension of the mimetic regime may describe any given cosmological model.

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