Can dark energy evolve to the Phantom

@article{Vikman2004CanDE,
  title={Can dark energy evolve to the Phantom},
  author={Alexander Vikman},
  journal={Physical Review D},
  year={2004},
  volume={71},
  pages={023515}
}
  • A. Vikman
  • Published 6 July 2004
  • Materials Science, Mathematics
  • Physical Review D
Dark energy with the equation of state $w(z)$ rapidly evolving from the dustlike ($w\ensuremath{\simeq}0$ at $z\ensuremath{\sim}1$) to the phantomlike ($\ensuremath{-}1.2\ensuremath{\lesssim}w\ensuremath{\lesssim}\ensuremath{-}1$ at $z\ensuremath{\simeq}0$) has been recently proposed as the best fit for the supernovae Ia data. Assuming that a dark energy component with an arbitrary scalar-field Lagrangian $p(\ensuremath{\varphi},{\ensuremath{\nabla}}_{\ensuremath{\mu}}\ensuremath{\varphi… 

Figures from this paper

Cosmological coincidence problem in interacting dark energy models

The interacting dark energy model with interaction term $Q={\ensuremath{\lambda}}_{m}H{\ensuremath{\rho}}_{m}+{\ensuremath{\lambda}}_{d}H{\ensuremath{\rho}}_{d}$ is considered. By studying the model

Phantom divide crossing with general non-minimal kinetic coupling

We propose a model of dark energy consists of a single scalar field with a general non-minimal kinetic couplings to itself and to the curvature. We study the cosmological dynamics of the equation of

Strong bounds on sum of neutrino masses in a 12 parameter extended scenario with non-phantom dynamical dark energy (w(z)≥-1\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek}

We obtained constraints on a 12 parameter extended cosmological scenario including non-phantom dynamical dark energy (NPDDE) with CPL parametrization. We also include the six

Distinguishing a rotating Kiselev black hole from a naked singularity using the spin precession of a test gyroscope

We study the critical values ($\alpha_{c}, a_{c}$) of the quintessential and spin parameters, to distinguish a rotating Kiselev black hole (RKBH) from a naked singularity. For any value of the

Effective actions for loop quantum cosmology in fourth-order gravity

Loop quantum cosmology (LQC) is a theory which renders the Big Bang initial singularity into a quantum bounce, by means of short-range repulsive quantum effects at the Planck scale. In this work, we

Cosmological perturbations in a mimetic matter model

We investigate the cosmological evolution of a mimetic matter model with arbitrary scalar potential. The cosmological reconstruction\char22{}which is the method for constructing a model for an

Minimally deformed wormholes

This work is devoted to the study of wormhole solutions in the framework of gravitational decoupling by means of the minimal geometric deformation scheme. As an example, to analyze how this

Strong bounds on sum of neutrino masses in a 12 parameter extended scenario with non-phantom dynamical dark energy ($$w(z)\ge -1$$w(z)≥-1)

We obtained constraints on a 12 parameter extended cosmological scenario including non-phantom dynamical dark energy (NPDDE) with CPL parametrization. We also include the six $$\Lambda $$ΛCDM

Reconstruction of general scalar-field dark energy models

The reconstruction of scalar-field dark energy models is studied for a general Lagrangian density $p(\ensuremath{\phi},X)$, where $X$ is a kinematic term of a scalar-field $\ensuremath{\phi}$. We

Constraints on holographic dark energy from type Ia supernova observations

In this paper, we use the type Ia supernovae data to constrain the holographic dark energy model proposed by Li. We also apply a cosmic age test to this analysis. We consider in this paper a
...

References

SHOWING 1-10 OF 31 REFERENCES

The state of the dark energy equation of state

By combining data from seven cosmic microwave background experiments (including the latest WMAP results) with the Hubble parameter measurement from the Hubble space telescope and luminosity

Can the dark energy equation - of - state parameter w be less than -1?

Models of dark energy are conveniently characterized by the equation-of-state parameter $w=p/\ensuremath{\rho},$ where $\ensuremath{\rho}$ is the energy density and p is the pressure. Imposing the

Cosmological Dynamics of Phantom Field

We study the general features of a dynamics of a phantom field in the cosmological context. In the case of an inverse coshyperbolic potential, we demonstrate that the phantom field can successfully

Constraints on dark energy from Chandra observations of the largest relaxed galaxy clusters

We present constraints on the mean matter density, {Omega}{sub m}, dark energy density, {Omega}{sub DE}, and the dark energy equation of state parameter, w, using Chandra measurements of the X-ray

Cosmological constraints on the dark energy equation of state and its evolution

We have calculated constraints on the evolution of the equation of state of the dark energy, w(z), from a joint analysis of data from the cosmic microwave background, large scale structure and

The case for dynamical dark energy revisited

We investigate the behaviour of dark energy using the recently released supernova data of Riess et al 2004 and a model independent parametrization for dark energy (DE). We find that, if no priors are

Uncorrelated estimates of dark energy evolution

Type Ia supernova data have recently become strong enough to enable, for the first time, constraints on the time variation of the dark energy density and its equation of state. Most analyses,

Foundations of observing dark energy dynamics with the Wilkinson Microwave Anisotropy Probe

Detecting dark energy dynamics is the main quest of current dark energy research. Addressing the issue demands a fully consistent analysis of cosmic microwave background, large-scale structure and

Braneworld models of dark energy

We explore a new class of braneworld models in which the scalar curvature of the (induced) brane metric contributes to the brane action. The scalar curvature term arises generically on account of

Quintessence, cosmic coincidence, and the cosmological constant

Recent observations suggest that a large fraction of the energy density of the Universe has negative pressure. One explanation is vacuum energy density; another is quintessence in the form of a