Higher dimensional phantom dark energy model ending at the de-Sitter phase

2021 ◽  
Author(s):  
Kangujam Priyokumar Singh ◽  
Pheiroijam Suranjoy Singh
Keyword(s):  
Dark Energy ◽  
Dark Energy Model ◽  
Energy Model ◽  
De Sitter ◽  
Higher Dimensional ◽  
Phantom Dark Energy

Exact solution of phantom dark energy model

2010 ◽  
Vol 19 (11) ◽  
pp. 119801 ◽  
Author(s):  
Wen-Fu Wang ◽  
Zheng-Wei Shui ◽  
Bin Tang
Keyword(s):  
Exact Solution ◽  
Dark Energy ◽  
Dark Energy Model ◽  
Energy Model ◽  
Phantom Dark Energy

scholarly journals Parametrization of Born-Infeld type phantom dark energy model

2009 ◽  
Vol 324 (1) ◽  
pp. 55-59
Author(s):  
Z. G. Huang ◽  
H. Q. Lu ◽  
W. Fang
Keyword(s):  
Dark Energy ◽  
Dark Energy Model ◽  
Energy Model ◽  
Phantom Dark Energy

scholarly journals LATE-TIME PHANTOM UNIVERSE IN SO(1, 1) DARK ENERGY MODEL WITH EXPONENTIAL POTENTIAL

2005 ◽  
Vol 20 (15) ◽  
pp. 1147-1154 ◽  
Author(s):  
YI-HUAN WEI
Keyword(s):  
Dark Energy ◽  
Dark Energy Model ◽  
Energy Model ◽  
Late Time ◽  
De Sitter ◽  
Exponential Potential ◽  
Coupling Energy ◽  
Expansion Phase ◽  
Perturbation Field ◽  
The Universe

We discuss the late-time property of universe and phantom field in the SO(1, 1) dark energy model for the potential V = V0e-βΦα with α and β two positive constants. We assume in advance some conditions satisfied by the late-time field to simplify equations, which are confirmed to be correct from the eventual results. For α < 2, the field falls exponentially off and the phantom equation of state rapidly approaches -1. When α = 2, the kinetic energy ρk and the coupling energy ρc become comparable but there is always ρk < -ρc so that the phantom property of field proceeds to hold. The analysis on the perturbation to the late-time field Φ illustrates the square effective mass of the perturbation field is always positive and thus the phantom is stable. The universe considered currently may evade the future sudden singularity and will evolve to de Sitter expansion phase.

STATEFINDER PARAMETERS FOR PHANTOM DARK ENERGY

2006 ◽  
Vol 21 (16) ◽  
pp. 1305-1311 ◽  
Author(s):  
PUXUN WU ◽  
HONGWEI YU
Keyword(s):  
Dark Energy ◽  
Dark Energy Model ◽  
Energy Model ◽  
Field Potentials ◽  
Statefinder Parameters ◽  
Phantom Field ◽  
Energy Models ◽  
Phantom Dark Energy ◽  
The Universe

The statefinder parameters were introduced recently to differentiate different dark energy models. In this paper we perform a statefinder diagnostic to the phantom dark energy model with two different phantom field potentials. Our results show that the statefinder diagnostic is rather robust in differentiating not only different dark energy models but also the same kind of models with different potentials which lead to different fate of the universe.

scholarly journals VariableGcorrection for dark energy model in higher dimensional cosmology

2012 ◽  
Vol 90 (4) ◽  
pp. 365-371 ◽  
Author(s):  
Shuvendu Chakraborty ◽  
Ujjal Debnath ◽  
Mubasher Jamil
Keyword(s):  
Dark Energy ◽  
Dark Energy Model ◽  
Energy Model ◽  
Higher Dimensional Cosmology ◽  
Higher Dimensional

COSMOLOGICAL DYNAMICS OF DILATONIC (PHANTOM) DARK ENERGY MODEL

2006 ◽  
Vol 15 (09) ◽  
pp. 1501-1514 ◽  
Author(s):  
Z. G. HUANG ◽  
H. Q. LU
Keyword(s):  
Dark Energy ◽  
Kinetic Energy ◽  
Dark Energy Model ◽  
Energy Model ◽  
Density Parameter ◽  
Late Time ◽  
Sufficient Condition ◽  
Phantom Model ◽  
Attractor Solution ◽  
Phantom Dark Energy

In this paper, we study the cosmological dynamics of dilatonic dark energy model and its phantom model — with negative kinetic energy. When the potential is taken as the form [Formula: see text], we investigate the existence of a late time attractor solution, and find out the sufficient condition. One interesting feature found by us is that the evolutions of components of comic density are locally fluctuating on the way to the late time attractor. But this local fluctuation cannot hold the trend that the equation of state ω evolves to -1 and the cosmic density parameter Ωσ evolves to 1, which are important features for a dark energy model that can meet the current observations.

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.

ATTRACTOR BEHAVIOR IN DILATONIC (PHANTOM) DARK ENERGY MODEL WITH POTENTIAL [1+(σ-A)2]e-Bσ

2006 ◽  
Vol 21 (39) ◽  
pp. 2977-2987
Author(s):  
Z. G. HUANG ◽  
H. Q. LU ◽  
W. FANG
Keyword(s):  
Dark Energy ◽  
Dark Energy Model ◽  
Energy Model ◽  
Fine Tuning ◽  
Density Parameter ◽  
Dilaton Field ◽  
Phantom Model ◽  
Attractor Solution ◽  
Phantom Dark Energy ◽  
M Theory

In this paper, we consider the dilatonic dark energy model and its phantom model. Based on the dilatonic (phantom) model, we take the potential of dilaton field of the form [1+(σ-A)2]e-Bσ which seems to connect with ideas from M-theory, and analyze the sufficient condition for the existence of attractor solution. We find that the behavior of the attractor is not sensitive to the initial condition, thus the fine-tuning problem is alleviated. By numerical analysis, we investigate the asymptotic behavior of the attractor, which corresponds to an equation of state ω = -1 and a cosmic density parameter Ωσ = 1.

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