Evolution of perturbations in the model of Tsallis holographic dark energy

Abstract

We investigated evolution of metric and density perturbations for Tsallis model of holographic dark energy with energy density $\sim L^{2\gamma -4}$, where $L$ is length of event horizon or inverse Hubble parameter and $\gamma$ is parameter of non-additivity close to $1$. Because holographic dark energy is not an ordinary cosmological fluid but a phenomena caused by boundaries of the universe, the ordinary analysis for perturbations is not suitable. One needs to consider perturbations of the future event horizon. For realistic values of parameters it was discovered that perturbations of dark energy don't grow infinitely but vanish or freeze. We also considered the case of realistic interaction between holographic dark energy and matter and showed that in this case perturbations also can asymptotically freeze with time.

arXiv comment14 p. 9 fig

References in corpus (51)

• Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
• Measurements of Omega and Lambda from 42 High-Redshift Supernovae
• Dynamics of dark energy
• The Cosmological Constant and Dark Energy
• Unified cosmic history in modified gravity: from F(R) theory to Lorentz non-invariant models
• Extended Theories of Gravity
• A Phantom Menace? Cosmological consequences of a dark energy component with super-negative equation of state
• Cosmological Constant - the Weight of the Vacuum
• Introduction to Modified Gravity and Gravitational Alternative for Dark Energy
• Modified Gravity Theories on a Nutshell: Inflation, Bounce and Late-time Evolution
• Dark Energy and the Accelerating Universe
• A Model of Holographic Dark Energy
• Effective Field Theory, Black Holes, and the Cosmological Constant
• Can the dark energy equation-of-state parameter w be less than -1?
• Quantum deSitter cosmology and phantom matter
• Quintessence: A Review
• Black hole thermodynamical entropy
• The final state and thermodynamics of dark energy universe
• Cosmological Dynamics of Phantom Field
• The Physics of Cosmic Acceleration
• Holographic Dark Energy
• Infrared cut-off proposal for the Holographic density
• Approaches to Understanding Cosmic Acceleration
• Tsallis Holographic Dark Energy
• Generalized entropy formalism and a new holographic dark energy model
• Black holes, cosmological solutions, future singularities, and their thermodynamical properties in modified gravity theories
• Constructing Phantom Cosmologies from Standard Scalar Field Universes
• New infrared cut-off for the holographic scalar fields models of dark energy
• K-Essential Phantom Energy: Doomsday around the corner?
• Covariant Generalized Holographic Dark Energy and Accelerating Universe
• Holographic dark energy through Tsallis entropy
• Modified cosmology from extended entropy with varying exponent
• Superquintessence
• Effective equation of state for dark energy: mimicking quintessence and phantom energy through a variable Lambda
• Generalized phantom energy
• Instability of holographic dark energy models
• Holographic inflation
• Tsallis holographic dark energy in the Brans-Dicke cosmology
• A Note on Tsallis Holographic Dark Energy
• Exorcising w < -1
• Avoidance of Big Rip In Phantom Cosmology by Gravitational Back Reaction
• Phantom Friedmann Cosmologies and Higher-Order Characteristics of Expansion
• Which cosmological model with dark energy -- phantom or LambdaCDM
• The Fate of Dark Energy
• Alleviating both $H_0$ and ${\sigma }_8$ tensions in Tsallis cosmology
• Cosmological perturbations in the Tsallis holographic dark energy scenarios
• Inflation driven by a holographic energy density
• Viscous fluid holographic inflation
• Induced gravity effect on inflationary parameters in an holographic cosmology
• Holographic correspondence of $F(R)$ gravity with/without matter fields
• Holographic bounds and Higgs inflation