Density perturbations in decaying holographic dark energy models

TL;DR

This paper investigates how holographic dark energy decaying into cold dark matter affects cosmological density perturbations, revealing that universe acceleration suppresses matter contrast growth regardless of IR cutoff choice.

Contribution

It introduces a model of interacting holographic dark energy with different IR cutoffs and analyzes the impact on density perturbations during universe acceleration and deceleration phases.

Findings

Density perturbations grow in decelerating universe with $\, ext{w}^{ m eff}>-1/3$.

Density perturbations decay in accelerating universe with $\, ext{w}^{ m eff}<-1/3$.

Acceleration suppresses the growth of matter contrast regardless of IR cutoff.

Abstract

We study cosmological perturbations in the context of an interacting dark energy model, where the holographic dark energy with IR cutoff decays into the cold dark matter (CDM). For this purpose, we introduce three IR cutoffs of Hubble horizon, particle horizon, and future event horizon. Here we present small perturbations under the case that effective equation of state (EOS: $\omega^{\rm eff}$) for the holographic energy density is determined to be the same negative constant as that for the CDM. Such new matter productions tend to dilute the density perturbations of CDM (matter contrast). For a decelerating universe of $\omega^{\rm eff}>-1/3$, the matter contrast is growing as the universe evolves, while for an accelerating universe of $\omega^{\rm eff}<-1/3$, the matter contrast is decaying, irrespective of the choice of IR cutoff. This shows clearly that the acceleration suppresses the growing of the density perturbations at the early universe.