scholarly journals Dark energy from a quintessence (phantom) field rolling near a potential minimum (maximum)

2009 ◽  
Vol 79 (10) ◽  
Author(s):  
Sourish Dutta ◽  
Emmanuel N. Saridakis ◽  
Robert J. Scherrer
Keyword(s):  
Dark Energy ◽  
Potential Minimum ◽  
Phantom Field

scholarly journals Dark energy from a phantom field near a local potential minimum

2009 ◽  
Vol 676 (1-3) ◽  
pp. 12-15 ◽  
Author(s):  
Sourish Dutta ◽  
Robert J. Scherrer
Keyword(s):  
Dark Energy ◽  
Local Potential ◽  
Potential Minimum ◽  
Phantom Field

scholarly journals STATEFINDER PARAMETERS FOR FIVE-DIMENSIONAL COSMOLOGY

2008 ◽  
Vol 23 (04) ◽  
pp. 269-279 ◽  
Author(s):  
BAORONG CHANG ◽  
HONGYA LIU ◽  
LIXIN XU ◽  
CHENGWU ZHANG
Keyword(s):  
Dark Energy ◽  
Statefinder Parameters ◽  
Phantom Field ◽  
Energy Models ◽  
Big Bounce

We study the statefinder parameter in the five-dimensional big bounce model, and apply it to differentiate the attractor solutions of quintessence and phantom field. It is found that the evolving trajectories of these two attractor solutions in the statefinder parameters plane are quite different, and that are different from the statefinder trajectories of other dark energy models.

scholarly journals Viscous dark energy and phantom field in an anisotropic universe

2014 ◽  
Vol 351 (1) ◽  
pp. 59-65 ◽  
Author(s):  
Hassan Amirhashchi ◽  
Anirudh Pradhan
Keyword(s):  
Dark Energy ◽  
Anisotropic Universe ◽  
Phantom Field

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 SOME CONSEQUENCES OF DARK ENERGY DENSITY VARYING EXPONENTIALLY WITH SCALE FACTOR

2005 ◽  
Vol 20 (36) ◽  
pp. 2805-2818
Author(s):  
SANIL UNNIKRISHNAN ◽  
T. R. SESHADRI
Keyword(s):  
Dark Energy ◽  
Energy Density ◽  
Cosmological Constant ◽  
Scale Factor ◽  
Dark Energy Density ◽  
Phantom Field

In this paper we have explored the consequences of a model of dark energy with its energy density varying exponentially with the scale factor. We first consider the model with ρϕ∝eκa, where κ is a constant. This is a kind of generalization of the cosmological constant model with κ=0. We show that such an exponentially varying dark energy density with the scale factor naturally leads to an equivalent phantom field. We also consider a model with ρϕ∝eκ/a and show that this also naturally leads to an equivalent phantom field.

scholarly journals Dark energy stars with a phantom field

2021 ◽  
Vol 103 (8) ◽  
Author(s):  
Muhammad F. A. R. Sakti ◽  
Anto Sulaksono
Keyword(s):  
Dark Energy ◽  
Phantom Field

scholarly journals Tracker phantom field and a cosmological constant: Dynamics of a composite dark energy model

2021 ◽  
Vol 104 (12) ◽  
Author(s):  
Francisco X. Linares Cedeño ◽  
Nandan Roy ◽  
L. Arturo Ureña-López
Keyword(s):  
Dark Energy ◽  
Cosmological Constant ◽  
Dark Energy Model ◽  
Energy Model ◽  
Phantom Field

scholarly journals The stochastic axiverse

2021 ◽  
Vol 2021 (9) ◽  
Author(s):  
Mario Reig
Keyword(s):  
Black Hole ◽  
Dark Energy ◽  
Decay Constant ◽  
Planck Scale ◽  
Potential Minimum ◽  
Long Period ◽  
Cmb Polarization ◽  
Axion Decay Constant ◽  
Axion Decay ◽  
Fundamental Requirement

Abstract In addition to spectacular signatures such as black hole superradiance and the rotation of CMB polarization, the plenitude of axions appearing in the string axiverse may have potentially dangerous implications. An example is the cosmological overproduction of relic axions and moduli by the misalignment mechanism, more pronounced in regions where the signals mentioned above may be observable, that is for large axion decay constant. In this work, we study the minimal requirements to soften this problem and show that the fundamental requirement is a long period of low-scale inflation. However, in this case, if the inflationary Hubble scale is lower than around O(100) eV, no relic DM axion is produced in the early Universe. Cosmological production of some axions may be activated, via the misalignment mechanism, if their potential minimum changes between inflation and today. As a particular example, we study in detail how the maximal-misalignment mechanism dilutes the effect of dangerous axions and allows the production of axion DM in a controlled way. In this case, the potential of the axion that realises the mechanism shifts by a factor ∆θ = π between the inflationary epoch and today, and the axion starts to oscillate from the top of its potential. We also show that axions with masses ma ∼ O(1 − 100) H0 realising the maximal-misalignment mechanism generically behave as dark energy with a decay constant that can take values well below the Planck scale, avoiding problems associated to super-Planckian scales. Finally, we briefly study the basic phenomenological implications of the mechanism and comment on the compatibility of this type of maximally-misaligned quintessence with the swampland criteria.

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