Averaging generalized scalar field cosmologies II: locally rotationally symmetric Bianchi I and flat Friedmann–Lemaître–Robertson–Walker models

Scalar field cosmologies with a generalized harmonic potential and a matter fluid with a barotropic equation of state (EoS) with barotropic index γ for the locally rotationally symmetric (LRS) Bianchi I and flat Friedmann–Lemaître–Robertson–Walker (FLRW) metrics are investigated. Methods from the th...

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Bibliographic Details
Published in:The European physical journal. C, Particles and fields Particles and fields, 2021-06, Vol.81 (6), p.1-26, Article 489
Main Authors: Leon, Genly, Cuéllar, Sebastián, González, Esteban, Lepe, Samuel, Michea, Claudio, Millano, Alfredo D.
Format: Article
Language:English
Subjects:
Algebra
Analysis
Astronomy
Astrophysics and Cosmology
Asymptotic properties
Cosmology
Elementary Particles
Equations of state
Hadrons
Heavy Ions
Mathematical models
Measurement Science and Instrumentation
Methods
Nonlinear systems
Nuclear Energy
Nuclear Physics
Numerical analysis
Parameters
Perturbation
Physics
Physics and Astronomy
Quantum Field Theories
Quantum Field Theory
Quintessence (cosmology)
Regular Article - Theoretical Physics
Scalars
Spacetime
String Theory
Time dependence
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Summary:Scalar field cosmologies with a generalized harmonic potential and a matter fluid with a barotropic equation of state (EoS) with barotropic index γ for the locally rotationally symmetric (LRS) Bianchi I and flat Friedmann–Lemaître–Robertson–Walker (FLRW) metrics are investigated. Methods from the theory of averaging of nonlinear dynamical systems are used to prove that time-dependent systems and their corresponding time-averaged versions have the same late-time dynamics. Therefore, the simplest time-averaged system determines the future asymptotic behavior. Depending on the values of γ , the late-time attractors of physical interests are flat quintessence dominated FLRW universe and Einstein-de Sitter solution. With this approach, the oscillations entering the system through the Klein–Gordon (KG) equation can be controlled and smoothed out as the Hubble parameter H – acting as time-dependent perturbation parameter – tends monotonically to zero. Numerical simulations are presented as evidence of such behavior.
ISSN:1434-6044
1434-6052
DOI:10.1140/epjc/s10052-021-09230-5