Evolution of perturbations in distinct classes of canonical scalar field models of dark energy

Abstract

Dark energy must cluster in order to be consistent with the equivalence principle. The background evolution can be effectively modelled by either a scalar field or by a barotropic fluid.The fluid model can be used to emulate perturbations in a scalar field model of dark energy, though this model breaks down at large scales. In this paper we study evolution of dark energy perturbations in canonical scalar field models: the classes of thawing and freezing models.The dark energy equation of state evolves differently in these classes.In freezing models, the equation of state deviates from that of a cosmological constant at early times.For thawing models, the dark energy equation of state remains near that of the cosmological constant at early times and begins to deviate from it only at late times.Since the dark energy equation of state evolves differently in these classes,the dark energy perturbations too evolve differently. In freezing models, since the equation of state deviates from that of a cosmological constant at early times, there is a significant difference in evolution of matter perturbations from those in the cosmological constant model.In comparison, matter perturbations in thawing models differ from the cosmological constant only at late times. This difference provides an additional handle to distinguish between these classes of models and this difference should manifest itself in the ISW effect.

11 pages, 6 figures, accepted for publication in Phys. Rev. D

References in corpus (26)

• Dynamics of dark energy
• Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
• Cosmology and the Fate of Dilatation Symmetry
• Dark Energy and Gravity
• The shape of the SDSS DR5 galaxy power spectrum
• Interacting holographic generalized Chaplygin gas model
• Interacting Holographic Phantom
• Holographic tachyon model of dark energy
• Structure formation in the presence of dark energy perturbations
• Parametrizations of the Dark Energy Density and Scalar Potentials
• Dark Energy: Mystery of the Millennium
• Gauge-invariant analysis of perturbations in Chaplygin gas unified models of dark matter and dark energy
• Tachyon dark energy models: dynamics and constraints
• The spherical collapse model and cluster formation beyond the $\Lambda$ cosmology: Indications for a clustered dark energy?
• Voids of dark energy
• The Evolution of Universe with th B-I Type Phantom Scalar Field
• Scalar Field Dark Energy Perturbations and their Scale Dependence
• Can cosmological observations uniquely determine the nature of dark energy ?
• The thawing dark energy dynamics: Can we detect it?
• A new perspective on the relation between dark energy perturbations and the late-time ISW effect
• Axionic dark energy and a composite QCD axion
• Probing Dark Energy at Galactic and Cluster Scales
• A mathematical analysis of the evolution of perturbations in a modified Chaplygin gas model
• Clustering Properties of Dynamical Dark Energy Models
• A comparison of perturbations in fluid and scalar field models of dark energy
• Colour entangled orphan quarks and dark energy from cosmic QCD phase transition

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• A new parametrization of dark energy equation of state leading to double exponential potential
• Scalar field dark energy perturbations and the Integrated Sachs Wolfe effect
• Evolution of Spherical Overdensity in Thawing Dark energy Models
• Perturbations in Tachyon Dark Energy and their Effect on Matter Clustering
• Tachyonic vs Quintessence dark energy: linear perturbations and CMB data
• Perturbations In Some Dark Energy Models
• Dark Energy Induced Anisotropy in Cosmic Expansion