Anisotropic Spacetimes in Chiral Scalar Field Cosmology

Abstract

Study the behaviour and the evolution of the cosmological field equations in an homogeneous and anisotropic spacetime with two scalar fields coupled in the kinetic term. Specifically, the kinetic energy for the scalar field Lagrangian is that of the Chiral model and defines a two-dimensional maximally symmetric space with negative curvature. For the background space we assume the locally rotational spacetime which describes the Bianchi I, the Bianchi III and the Kantowski-Sachs anisotropic spaces. We work on the $H$% -normalization and we investigate the stationary points and their stability. For the exponential potential we find a new exact solution which describes an anisotropic inflationary solution. The anisotropic inflation is always unstable, while future attractors are the scaling inflationary solution or the hyperbolic inflation. For scalar field potential different from the exponential, the de Sitter universe exists.

arXiv comment17 pages, 2 figures, published in Eur. Phys. J. Plus

References in corpus (50)

• Exponential potentials and cosmological scaling solutions
• Quintom Cosmology: Theoretical implications and observations
• Super-Horizon Scale Dynamics of Multi-Scalar Inflation
• Perturbations in generalized multi-field inflation
• Generating the curvature perturbation at the end of inflation
• Primordial Bispectrum from Multifield Inflation with Nonminimal Couplings
• Multiple field inflation
• Quintom cosmologies with arbitrary potentials
• The Dynamics of Multi-Scalar Field Cosmological Models and Assisted Inflation
• Hyperinflation
• Dynamical analysis of generalized Galileon cosmology
• Cosmological behavior in extended nonlinear massive gravity
• Dynamical analysis of anisotropic scalar-field cosmologies for a wide range of potentials
• Two scalar field cosmology: Conservation laws and exact solutions
• Primordial perturbations from inflation with a hyperbolic field-space
• Dynamical systems analysis of anisotropic cosmologies in $R^n$-gravity
• Tensor-multi-scalar theories from multidimensional cosmology
• Angular inflation in multi-field $\alpha$-attractors
• Out of the Swampland with Multifield Quintessence?
• Exact Solutions in Chiral Cosmology
• New accelerating solutions in late-time cosmology
• Dynamics in Varying vacuum Finsler-Randers Cosmology
• Kantowski-Sachs Einstein-æther perfect fluid models
• Anisotropic Cosmological Model in Modified Brans--Dicke Theory
• Primordial Anisotropies in Gauged Hybrid Inflation
• Power Spectra beyond the Slow Roll Approximation in Theories with Non-Canonical Kinetic Terms
• Qualitative analysis of Kantowski-Sachs metric in a generic class of $f(R)$ models
• Hyperbolic field space and swampland conjecture for DBI scalar
• Kantowski-Sachs Einstein-Aether Scalar Field Cosmological Models
• Cosmological Solutions in Multiscalar Field Theory
• Dynamics of Chiral Cosmology
• The Behavior of Kasner Cosmologies with Induced Matter
• Szekeres Universes with Homogeneous Scalar Fields
• Stochastic Effects in Anisotropic Inflation
• Pure Lovelock Kasner metrics
• Spatially self-similar locally rotationally symmetric perfect fluid models
• Primordial curvature perturbation during and at the end of multi-field inflation
• Integrable modified gravity cosmological models with an additional scalar field
• Classical and quantum exact solutions for a FRW in chiral like cosmology
• Dynamical Analysis of Anisotropic Inflation
• Hubble multi-scalar inflation
• Extended analysis for the Evolution of the Cosmological history in Einstein-aether Scalar Field theory
• Exact Kantowski-Sachs spacetimes in Einstein-Aether Scalar field theory
• Multi-scalar field cosmology from SFT: an exactly solvable approximation
• Unified dark matter and dark energy description in a chiral cosmological model
• Anisotropic chiral cosmology: exact solutions
• General solutions to $\mathcal{N}$-field cosmology with exponential potentials
• New Anisotropic Exact Solution in Multifield Cosmology
• Dynamics of tilted Bianchi models of types III, IV, V in presence of diffusion
• Stabilising the Planck mass shortly after inflation