Cosmological model involving an interacting van der Waals fluid

Abstract

A model for the late-time accelerated expansion of the universe is considered where a van der Waals fluid interacting with matter plays the role of dark energy. The transition towards this phase in the cosmic evolution history is discussed in detail and, moreover, a complete classification of the future finite-time singularities is obtained for six different possible forms of the non-gravitational interaction between dark energy (the van der Waals fluid) and dark matter. This study shows, in particular, that a universe with a non-interacting three-parameter van der Waals fluid can evolve into a universe characterized by a Type IV~(Generalized Sudden) Singularity. On the other hand, for certain values of the parameters, exit from the accelerated expanding phase is possible in the near future, what means that the expansion of the universe in the future could become decelerated. On the other hand, our study shows that space can be divided into different regions. For some of them, in particular, the non-gravitational interactions $Q=3Hb{\rho }_{de}$, $Q=3Hb{\rho }_{dm}$ and $Q=3Hb({\rho }_{de}+{\rho }_{de})$ may completely suppress future finite-time singularity formation, for sufficiently high values of $b$. On the other hand, for some other regions of the parameter space, the mentioned interactions would not affect the singularity type, namely the Type IV singularity generated in the case of the non-interacting model would be preserved. A similar conclusion has been archived for the cases of $Q=3bH{\rho }_{de}{\rho }_{dm}/({\rho }_{de}+{\rho }_{dm})$, $Q=3bH{\rho }_{dm}^2/({\rho }_{de}+{\rho }_{dm})$ and $Q=3bH{\rho }_{de}^2/({\rho }_{de}+{\rho }_{dm})$ non-gravitational interactions, with only one difference: the $Q=3bH{\rho }_{dm}^2/({\rho }_{de}+{\rho }_{dm})$ interaction will change the Type IV singularity of the non-interacting model into a Type II~(The Sudden) singularity.

References in corpus (65)

• Unified cosmic history in modified gravity: from F(R) theory to Lorentz non-invariant models
• Modified Gravity and Cosmology
• Extended Theories of Gravity
• A Phantom Menace? Cosmological consequences of a dark energy component with super-negative equation of state
• Introduction to Modified Gravity and Gravitational Alternative for Dark Energy
• Modified Gravity Theories on a Nutshell: Inflation, Bounce and Late-time Evolution
• Phantom Energy and Cosmic Doomsday
• Modified gravity with negative and positive powers of the curvature: unification of the inflation and of the cosmic acceleration
• f(T) teleparallel gravity and cosmology
• Properties of singularities in (phantom) dark energy universe
• Late-time cosmology in (phantom) scalar-tensor theory: dark energy and the cosmic speed-up
• Modified f(R) gravity consistent with realistic cosmology: from matter dominated epoch to dark energy universe
• Unifying phantom inflation with late-time acceleration: scalar phantom-non-phantom transition model and generalized holographic dark energy
• Class of viable modified $f(R)$ gravities describing inflation and the onset of accelerated expansion
• Cosmological viability of f(R)-gravity as an ideal fluid and its compatibility with a matter dominated phase
• Sudden Future Singularities
• Observational constraints on dark energy with generalized equations of state
• Future of the universe in modified gravitational theories: Approaching to the finite-time future singularity
• Further stable neutron star models from f(R) gravity
• Inflationary cosmology in modified gravity theories
• Stable dark energy stars
• Phantom scalar dark energy as modified gravity: understanding the origin of the Big Rip singularity
• Extreme neutron stars from Extended Theories of Gravity
• Gaussian Process Cosmography
• LambdaCDM epoch reconstruction from F(R,G) and modified Gauss-Bonnet gravities
• Viscous Little Rip Cosmology
• Theoretical Models of Dark Energy
• More General Sudden Singularities
• Compact stars in $f(R,T)$ gravity
• The realistic models of relativistic stars in f(R) = R + alpha R^2 gravity
• Worse than a big rip?
• Bouncing cosmology with future singularity from modified gravity
• Modified TOV in gravity's rainbow: properties of neutron stars and dynamical stability conditions
• Singular Inflationary Universe from $F(R)$ Gravity
• Cosmological models described by a mixture of van der Waals fluid and dark energy
• Barotropic index w-singularities in cosmology
• Unifying inflation with dark energy in modified F(R) Horava-Lifshitz gravity
• $f(T)$ gravitational baryogenesis
• What are $Om{h}^2(z_1,z_2)$ and $Om(z_1,z_2)$ diagnostics telling us in light of $H(z)$ data?
• Theoretical Limits on the Equation-of-State Parameter of Phantom Cosmology
• Beyond the perfect fluid hypothesis for dark energy equation of state
• Anisotropic cosmological models with perfect fluid and dark energy revisited
• Constraining Van der Waals quintessence by observations
• Interacting Quintessence Models of Dark Energy
• Inflationary universe in terms of a van der Waals viscous fluid
• New holographic reconstruction of scalar field dark energy models in the framework of chameleon Brans-Dicke cosmology
• Compact objects in Horndeski gravity
• Interacting Ghost Dark Energy Models with Variable $G$ and $\Lambda$
• Hidden past of dark energy cosmological models
• Exotic-singularity-driven dark energy
• Observational constraints on cosmological future singularities
• On a holographic dark energy model with a Nojiri-Odintsov cut-off in general relativity
• Beyond-one-loop quantum gravity action yielding both inflation and late-time acceleration
• Neutron Stars in Screened Modified Gravity: Chameleon vs Dilaton
• Interacting two-component fluid models with varying EoS parameter
• Singular $F(R)$ Cosmology Unifying Early and Late-time Acceleration with Matter and Radiation Domination Era
• Interacting varying Ghost Dark energy models in General Relativity
• Phenomenological Fluids from Interacting Tachyonic Scalar Fields
• Brane cosmology with a van der Waals equation of state
• On a phenomenology of the accelerated expansion with a varying ghost dark energy
• Lyth bound revisited
• Inflationary Universe with a Viscous Fluid Avoiding Self-Reproduction
• Effects of Finite-time Singularities on Gravitational Waves
• The van der Waals fluid and its role in cosmology
• Mutually interacting Tachyon dark energy with variable $G$ and $\Lambda$

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• Dynamical Systems Perspective of Cosmological Finite-time Singularities in $f(R)$ Gravity and Interacting Multifluid Cosmology
• Finite-time Cosmological Singularities and the Possible Fate of the Universe
• An analysis of the $H_0$ tension problem in a universe with a viscous dark fluid
• Swampland criteria for a dark-energy dominated universe, ensuing from Gaussian process and H(z) data analysis
• A Study of Finite-time Singularities of Loop Quantum Cosmology Interacting Multifluids
• Constraining $f(Q,L_m)$ gravity with bulk viscosity
• Bulk viscous cosmological model in $f(R,T)$ theory of gravity
• Diffusion in unimodular gravity: Analytical solutions, late-time acceleration, and cosmological constraints
• The Classical and Loop Quantum Cosmology Phase Space of Interacting Dark Energy and Superfluid Dark Matter
• Solving the $H_0$ tension in $f(T)$ Gravity through Bayesian Machine Learning
• Cosmological Einstein-Maxwell model with $g$-essence
• Analysis cosmological tachyon and fermion model and observation data constraints
• Thermodynamic analysis for Non-linear system (Van-der-Waals EOS) with viscous cosmology
• Thermodynamics and energy condition analysis for Van-Der-Waals EOS without viscous cosmology