Sensitivity of quintessence perturbations to initial conditions

@article{Liu2004SensitivityOQ,
  title={Sensitivity of quintessence perturbations to initial conditions},
  author={Jingsong Liu},
  journal={Physical Review D},
  year={2004},
  volume={69},
  pages={083504}
}
  • Jingsong Liu
  • Published 28 February 2004
  • Physics
  • Physical Review D
Gauge invariant quintessence perturbations in the quintessence and cold dark matter (QCDM) model are investigated. For three cases of constant equation-of-state (EOS) parameter, linear scalar field potential, and supergravity scalar field potential, their perturbation evolutions have a similar dependence on EOS parameter and scale, but they have different sensitivity to the initial conditions due to the different shapes of the quintessence potential. They have a minor effect on primary CMB… Expand
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References

SHOWING 1-10 OF 27 REFERENCES
Exhaustive Study of Cosmic Microwave Background Anisotropies in Quintessential Scenarios
Recent high-precision measurements of the CMB anisotropies performed by the BOOMERanG and MAXIMA-1 experiments provide an unmatched set of data allowing us to probe different cosmological models.Expand
Quintessential Cosmology Novel Models of Cosmological Structure Formation
We examine the possibility that a substantial fraction of the total energy density in a spatially flat Universe is composed of a time-dependent and spatially inhomogeneous component whoseExpand
Evolution of large-scale perturbations in quintessence models
We carry out a comprehensive study of the dynamics of large-scale perturbations in quintessence scenarios. We model the contents of the Universe by a perfect fluid with equation of state w_f and aExpand
Sensitivity of the cosmic microwave background anisotropy to initial conditions in quintessence cosmology
We analyze the evolution of energy density fluctuations in cosmological scenarios with a mixture of cold dark matter and quintessence, in which the quintessence field is modeled by a constantExpand
Cosmological consequences of a rolling homogeneous scalar field.
  • Ratra, Peebles
  • Physics, Medicine
  • Physical review. D, Particles and fields
  • 1988
TLDR
It is argued that a number of models in which the energy density of the scalar field red-shifts in a specific manner are studied could reconcile the low dynamical estimates of the mean mass density with the negligibly small spatial curvature preferred by inflation. Expand
Gauge invariant perturbation analysis for quintessence with an exponential potential
Adiabatic perturbations in the cosmology of a quintessential scalar field with exponential potential gravitationally coupled to radiation/matter are investigated in a gauge invariant formalism. TheExpand
Theory of cosmological perturbations
We present in a manifestly gauge-invariant form the theory of classical linear gravitational perturbations in part I, and a quantum theory of cosmological perturbations in part II. Part I includesExpand
Discretuum versus continuum dark energy
Abstract The dark energy equation of state for theories with either a discretuum or continuum distribution of vacua is investigated. In the discretuum case the equation of state is constant w = p / ρExpand
Gauge Invariant Cosmological Perturbations
The physical interpretation of perturbations of homogeneous, isotropic cosmological models in the early Universe, when the perturbation is larger than the particle horizon, is clarified by defining aExpand
Supergravity, Dark Energy and the Fate of the Universe
We propose a description of dark energy and acceleration of the universe in extended supergravities with de Sitter (dS) solutions. Some of them are related to M-theory with non-compact internalExpand
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