scholarly journals Ricci dark energy in bumblebee gravity model

2019 ◽  
Vol 34 (22) ◽  
pp. 1950171 ◽  
Author(s):  
W. D. R. Jesus ◽  
A. F. Santos
Keyword(s):  
Dark Energy ◽  
Holographic Dark Energy ◽  
Friedmann Equation ◽  
Gravitational Theory ◽  
Coupling Constant ◽  
Ricci Dark Energy ◽  
Dark Energy Density ◽  
Energy Models ◽  
First Case ◽  
Lorentz Symmetry Breaking

The Ricci dark energy is a model inspired by the holographic dark energy models with the dark energy density being proportional to Ricci scalar curvature. Here, this model is studied in the bumblebee gravity theory. It is a gravitational theory that exhibit spontaneous Lorentz symmetry breaking. Then, the modified Friedmann equation is solved for two cases. In the first case, the coupling constant [Formula: see text] is equal to zero and in the second case a solution in the vacuum, where the bumblebee field becomes a constant that minimizes the potential, is considered. The coupling constant controls the interaction gravity-bumblebee.

scholarly journals POWER-LAW ENTROPY CORRECTED NEW HOLOGRAPHIC SCALAR FIELD MODELS OF DARK ENERGY WITH MODIFIED IR-CUTOFF

2011 ◽  
Vol 26 (33) ◽  
pp. 2487-2499 ◽  
Author(s):  
A. KHODAM-MOHAMMADI
Keyword(s):  
Dark Energy ◽  
Scalar Field ◽  
Kinetic Energy ◽  
Holographic Dark Energy ◽  
Matter Field ◽  
Dark Energy Density ◽  
Energy Models ◽  
Scalar Field Models ◽  
Phantom Barrier ◽  
Limiting Case

In this work, the PLECHDE model with Granda–Oliveros (G–O) IR-cutoff is studied. The evolution of dark energy density, deceleration and EoS parameters are calculated. I demonstrate that under a condition, our universe can accelerate near the phantom barrier at present time. We calculate these parameters also in PLECHDE at Ricci scale, when α = 2 and β = 1, and a comparison between Ricci scale, G–O cutoff and non-corrected HDE without matter field with G–O cutoff is done. The correspondence between this model and some scalar field of dark energy models is established. By this method, the evolutionary treatment of kinetic energy and potential for quintessence, tachyon, K-essence and dilaton fields, are obtained. I show that the results has a good compatibility with previous work in the limiting case of flat, dark dominated and non-corrected holographic dark energy.

scholarly journals STATEFINDER DIAGNOSTIC FOR DARK ENERGY MODELS IN BIANCHI I UNIVERSE

2012 ◽  
Vol 21 (05) ◽  
pp. 1250046 ◽  
Author(s):  
M. SHARIF ◽  
RABIA SALEEM
Keyword(s):  
Dark Energy ◽  
Holographic Dark Energy ◽  
Chaplygin Gas ◽  
Accelerated Expansion ◽  
Ricci Dark Energy ◽  
Generalized Chaplygin Gas ◽  
Bianchi I ◽  
Energy Models ◽  
Expansion Of The Universe ◽  
The Universe

In this paper, we investigate the statefinder, the deceleration and equation of state parameters when universe is composed of generalized holographic dark energy or generalized Ricci dark energy for Bianchi I universe model. These parameters are found for both interacting as well as noninteracting scenarios of generalized holographic or generalized Ricci dark energy with dark matter and generalized Chaplygin gas. We explore these parameters graphically for different situations. It is concluded that these models represent accelerated expansion of the universe.

scholarly journals Some models of holographic dark energy on the Randall–Sundrum brane and observational data

2019 ◽  
Vol 29 (01) ◽  
pp. 1950176 ◽  
Author(s):  
A. V. Astashenok ◽  
A. S. Tepliakov
Keyword(s):  
Dark Energy ◽  
Energy Density ◽  
Observational Data ◽  
Energy Analysis ◽  
Holographic Dark Energy ◽  
Brane Tension ◽  
Dark Energy Density ◽  
Energy Models ◽  
Current Energy ◽  
The Universe

Some models of holographic dark energy for Randall–Sundrum brane are considered. For the first class of dark energy models, we take energy density in the form [Formula: see text], where [Formula: see text] is size of event horizon in universe and [Formula: see text] is parameter (Tsallis holographic energy). Analysis of observational data allows to define upper limit on value of [Formula: see text] ([Formula: see text] is current energy density in the universe and [Formula: see text] is brane tension). Then we investigate models for which dark energy density has the form [Formula: see text] where [Formula: see text] is Hubble parameter.

Viewing the Cosmological Consequences of Modified Holographic Dark Energy in Various Interaction Scenarios

2018 ◽  
Vol 73 (3) ◽  
pp. 251-257 ◽  
Author(s):  
Sthiti Chakrabarti ◽  
Surajit Chattopadhyay
Keyword(s):  
Dark Energy ◽  
Holographic Dark Energy ◽  
State Parameter ◽  
Scale Factor ◽  
Matter Density ◽  
Ricci Dark Energy ◽  
Dark Energy Density ◽  
Interaction Terms ◽  
Scale Factors ◽  
Phantom Phase

AbstractIn the work reported here, we have considered the interaction between modified holographic Ricci dark energy, a particular choice of Nojiri–Odintsov cut-offs, and pressureless dark matter for three different choices of scale factor, namely logamediate, intermediate, and emergent. Two different interaction terms have been considered. In one case, the interaction has been taken proportional to the dark energy density; in the other case, it has been taken proportional to the matter density. In the case of Q=3Hδρx, we have observed that there is a crossing of phantom boundary and the equation of state parameter has been observed to behave like quintessence. The influence of various parameters in the scale factors has also been observed. Also, an exit from phantom phase has been observed for the choice of scale factor in the emergent form. Considering the interaction term Q to be proportional to the matter density for logamediate scale factor, wx has been found to behave like quintessence, i.e. >−1. For the emergent scale factor in this interaction scenario, the model has been found to lead to a wx parameter lying in the region ≤−1. Therefore, in general, it has been found that Q=3Hδρx is more suitable than Q=3Hδρm in creating a model having a wx parameter crossing the phantom boundary.

scholarly journals Physical Acceptability of the Renyi, Tsallis and Sharma-Mittal Holographic Dark Energy Models in the f(T,B) Gravity under Hubble’s Cutoff

Universe ◽  
2021 ◽  
Vol 7 (3) ◽  
pp. 67
Author(s):  
Salim Harun Shekh ◽  
Pedro H. R. S. Moraes ◽  
Pradyumn Kumar Sahoo
Keyword(s):  
Dark Energy ◽  
Holographic Dark Energy ◽  
Cosmological Parameters ◽  
Field Equations ◽  
Eos Parameter ◽  
Two Fluids ◽  
Gravitational Field Equations ◽  
Energy Models ◽  
Different Types ◽  
The Universe

In the present article, we investigate the physical acceptability of the spatially homogeneous and isotropic Friedmann–Lemâitre–Robertson–Walker line element filled with two fluids, with the first being pressureless matter and the second being different types of holographic dark energy. This geometric and material content is considered within the gravitational field equations of the f(T,B) (where T is the torsion scalar and the B is the boundary term) gravity in Hubble’s cut-off. The cosmological parameters, such as the Equation of State (EoS) parameter, during the cosmic evolution, are calculated. The models are stable throughout the universe expansion. The region in which the model is presented is dependent on the real parameter δ of holographic dark energies. For all δ≥4.5, the models vary from ΛCDM era to the quintessence era.

scholarly journals Sandage–Loeb test for the new agegraphic and Ricci dark energy models

2010 ◽  
Vol 691 (1) ◽  
pp. 11-17 ◽  
Author(s):  
Jingfei Zhang ◽  
Li Zhang ◽  
Xin Zhang
Keyword(s):  
Dark Energy ◽  
Ricci Dark Energy ◽  
Energy Models

Holographic dark energy in a vector field cosmology

2015 ◽  
Vol 12 (10) ◽  
pp. 1550119 ◽  
Author(s):  
S. Davood Sadatian
Keyword(s):  
Dark Energy ◽  
Vector Field ◽  
Equation Of State ◽  
Energy Density ◽  
Holographic Dark Energy ◽  
Lorentz Invariance ◽  
Holographic Model ◽  
Dark Energy Density ◽  
Invariance Violation ◽  
Lorentz Invariance Violation

We obtain interacting holographic dark energy density in the framework of vector field cosmology (LIV). We consider possible modification of equation of state for the holographic energy density in lorentz invariance violation cosmology. In this case we select Jeans length as the IR cut-off in the holographic model. Then we consider the interaction between holographic energy densities ρΛ and ρm in this framework.

Power Law and Logarithmic Entropy Corrected Ricci Dark Energy Models in Brans-Dicke Chameleon Cosmology

2013 ◽  
Vol 53 (2) ◽  
pp. 566-578 ◽  
Author(s):  
Antonio Pasqua ◽  
Khudhair A. Assaf ◽  
Ayman A. Aly
Keyword(s):  
Dark Energy ◽  
Power Law ◽  
Ricci Dark Energy ◽  
Energy Models

scholarly journals Study of Thermodynamics in Generalized Holographic and Ricci Dark Energy Models

2011 ◽  
Vol 51 (2) ◽  
pp. 577-588 ◽  
Author(s):  
Samarpita Bhattacharya ◽  
Ujjal Debnath
Keyword(s):  
Dark Energy ◽  
Ricci Dark Energy ◽  
Energy Models
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