On the growth of perturbations in interacting dark energy and dark matter fluids

Abstract

The covariant generalizations of the background dark sector coupling suggested in G. Mangano, G. Miele and V. Pettorino, Mod. Phys. Lett. A 18, 831 (2003) are considered. The evolution of perturbations is studied with detailed attention to interaction rate that is proportional to the product of dark matter and dark energy densities. It is shown that some classes of models with coupling of this type do not suffer from early time instabilities in strong coupling regime.

11 pages, 2 figures. v3: minor changes, typos fixed

References in corpus (10)

• Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
• Cosmological Constraints from the SDSS Luminous Red Galaxies
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• Dynamics of interacting dark energy
• Stability of the curvature perturbation in dark sectors' mutual interacting models
• Observational constraints on an interacting dark energy model
• Dark Interactions and Cosmological Fine-Tuning
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• On the large-scale instability in interacting dark energy and dark matter fluids

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• Cosmological constraints on interacting dark energy with redshift-space distortion after Planck data
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• Finite-time Cosmological Singularities and the Possible Fate of the Universe
• Testing coupled dark energy with large scale structure observation
• Coupled dark energy with perturbed Hubble expansion rate
• Cosmological constraints on coupled dark energy
• Probing the imprint of interacting dark energy on very large scales
• Distinguishing interacting dark energy from wCDM with CMB, lensing, and baryon acoustic oscillation data
• Holographic Dark Energy from Fluid/Gravity Duality Constraint by Cosmological Observations
• Constraints on a decomposed dark fluid with constant adiabatic sound speed by jointing the geometry test and growth rate after Planck data
• Flat limits of curved interacting cosmic fluids
• Singularities in cosmologies with interacting fluids
• Perturbation level interacting dark energy model and its consequence on late-time cosmological parameters