2019
DOI: 10.1142/s0218271819501104
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Dissipative unified dark fluid model

Abstract: We consider a unified dissipative dark fluid model. Our fluid contains an adiabatic part plus a bulk viscous one. The adiabatic part has the ability to asymptote between two power laws and so can interpolate between the dust and dark energy equations of state at early and late times. The dissipative part is a bulk viscous part with constant viscosity coefficient. The model is analyzed using the phase space methodology which helps to understand the dynamical behavior of the model in a robust manner without refe… Show more

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Cited by 8 publications
(6 citation statements)
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“…The new inflation cosmic model set by Andrei Linde, Andreas Albrecht and Paul Steinhardt, et al is basically consistent with the initial conditions of the universe in the original model of inflationary universe [50][55] [56] . In order to obtain a new inflationary cosmological model, Linde, Albrecht and Steinhardt et al require particle physics theory to contain a scalar field φ , and have the following properties [50][55] [56] : (i) the effective potential function V ( φ ) must have a minimum at φ ≠ 0 ; (ii) V ( φ ) must be very flat near φ = 0, and it is usually assumed that at φ = 0 It is a local maximum of V ( φ ); (iii) at high temperature T, the heat equilibrium value of φ, i.e. the minimum of the effective potential V T ( φ, T ) at finite temperature must be at φ = 0.…”
Section: Model (I) Of Super-inflating Universe With Big Impetusmentioning
confidence: 70%
See 3 more Smart Citations
“…The new inflation cosmic model set by Andrei Linde, Andreas Albrecht and Paul Steinhardt, et al is basically consistent with the initial conditions of the universe in the original model of inflationary universe [50][55] [56] . In order to obtain a new inflationary cosmological model, Linde, Albrecht and Steinhardt et al require particle physics theory to contain a scalar field φ , and have the following properties [50][55] [56] : (i) the effective potential function V ( φ ) must have a minimum at φ ≠ 0 ; (ii) V ( φ ) must be very flat near φ = 0, and it is usually assumed that at φ = 0 It is a local maximum of V ( φ ); (iii) at high temperature T, the heat equilibrium value of φ, i.e. the minimum of the effective potential V T ( φ, T ) at finite temperature must be at φ = 0.…”
Section: Model (I) Of Super-inflating Universe With Big Impetusmentioning
confidence: 70%
“…Therefore, in the later model, scalar field φ is a gauge singlet, called an expander. In most cases, this field only promotes inflation, and all models based on slow roll phase transition are called new inflation cosmic models [50][55] [56] .…”
Section: Model (I) Of Super-inflating Universe With Big Impetusmentioning
confidence: 99%
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“…Some physicists regard background independence as a basic requirement for a theory of quantum gravity. It is especially true since general relativity has been background independent [132]- [133] .…”
Section: Basic Equation Of Cosmic Paradigm Dynamicsmentioning
confidence: 99%