Hubble parameter corrected interactions in cosmology

Abstract

In this paper we make steps in a new direction by considering fluids with EoS of more general form $F(\rho ,P)=0$. It is thought that there should be interaction between cosmic fluids, but this assumption for this stage carries only phenomenological character opening a room for different kind of manipulations. In this article we will consider a modification of an interaction $Q$, where we accept that interaction parameter $b_1$ (order of unity) in $Q=3H{b}_1\rho$ is time dependent and presented as a linear function of Hubble parameter $H$ of the form $b_0+btH$, where $b$ and $b_0$ are constants. We consider two different models include modified Chaplygin gas and palotropic gas which have bulk viscosity. Then, we investigate problem numerically and analyze behavior of different cosmological parameters concerning to fluids and behavior of Universe.

21 pages. Comparison with observational data added in new version

References in corpus (8)

• Cosmological constant and vacuum energy: old and new ideas
• Hubble expansion and structure formation in the "running FLRW model" of the cosmic evolution
• Entropic-force dark energy reconsidered
• Effective equation of state for running vacuum: "mirage" quintessence and phantom dark energy
• Latest Observational Constraints to the Ghost Dark Energy Model by Using Markov Chain Monte Carlo Approach
• Interacting varying Ghost Dark energy models in General Relativity
• Phenomenological Varying Modified Chaplygin Gas with Variable $G$ and $\Lambda$: Toy Models for Our Universe
• Interaction between Generalized Varying Chaplygin gas and Tachyonic Fluid