scholarly journals Holographic dark energy with non-minimal derivative coupling to gravity effects

2020 ◽  
Vol 30 ◽  
pp. 100712
Author(s):  
Chonticha Kritpetch ◽  
Candrasyah Muhammad ◽  
Burin Gumjudpai
Keyword(s):  
Dark Energy ◽  
Holographic Dark Energy ◽  
Derivative Coupling ◽  
Gravity Effects

scholarly journals Barrow holographic dark energy

2020 ◽  
Vol 102 (12) ◽  
Author(s):  
Emmanuel N. Saridakis
Keyword(s):  
Dark Energy ◽  
Holographic Dark Energy

scholarly journals Tsallis holographic dark energy for inflation

2021 ◽  
Vol 103 (8) ◽  
Author(s):  
Abolhassan Mohammadi ◽  
Tayeb Golanbari ◽  
Kazuharu Bamba ◽  
Iarley P. Lobo
Keyword(s):  
Dark Energy ◽  
Holographic Dark Energy

scholarly journals Rényi holographic dark energy in higher dimension Cosmology

2021 ◽  
Vol 426 ◽  
pp. 168403
Author(s):  
A. Saha ◽  
S. Ghose ◽  
A. Chanda ◽  
B.C. Paul
Keyword(s):  
Dark Energy ◽  
Holographic Dark Energy ◽  
Higher Dimension

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.

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