Parametrization of Born-Infeld type phantom dark energy model

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.

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

Chinese Journal of Physics ◽

10.1016/j.cjph.2021.05.022 ◽

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

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COSMOLOGICAL DYNAMICS OF DILATONIC (PHANTOM) DARK ENERGY MODEL

International Journal of Modern Physics D ◽

10.1142/s0218271806008863 ◽

2006 ◽

Vol 15 (09) ◽

pp. 1501-1514 ◽

Cited By ~ 10

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.

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Attractor behavior in dilatonic (phantom) dark energy model with an especial potential

Journal of Shanghai University (English Edition) ◽

10.1007/s11741-008-0605-1 ◽

2008 ◽

Vol 12 (6) ◽

pp. 489-494

Author(s):

Chen-xing Wei ◽

Hui-qing Lu ◽

Jian-hua Zhou

Keyword(s):

Dark Energy ◽

Dark Energy Model ◽

Energy Model ◽

Phantom Dark Energy

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Logarithmic entropy corrected holographic dark energy with nonminimal kinetic coupling

Canadian Journal of Physics ◽

10.1139/p11-140 ◽

2012 ◽

Vol 90 (1) ◽

pp. 61-66 ◽

Cited By ~ 8

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.

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

Modern Physics Letters A ◽

10.1142/s0217732306020548 ◽

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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