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Scalar field in Bianchi type-I cosmology with Lyra's geometry

Evgeny Petuhov, Bijan Saha

Abstract

In this study, we examine the role of a scalar field in the evolution of the Universe within the framework of a Bianchi type-I cosmological model with Lyra's geometry. Previous research has explored the nonlinear spinor field in various anisotropic and isotropic cosmological models. In our current study, we and dynamical restrictions for Lyra parameters and violation of stress-energy tensor conservation within Lyra geometry. We shown that in considering cases behavior of Lyra's parameter corresponds to relative in?uence in early universe and absence of Lyra geometry in present universe.

Scalar field in Bianchi type-I cosmology with Lyra's geometry

Abstract

In this study, we examine the role of a scalar field in the evolution of the Universe within the framework of a Bianchi type-I cosmological model with Lyra's geometry. Previous research has explored the nonlinear spinor field in various anisotropic and isotropic cosmological models. In our current study, we and dynamical restrictions for Lyra parameters and violation of stress-energy tensor conservation within Lyra geometry. We shown that in considering cases behavior of Lyra's parameter corresponds to relative in?uence in early universe and absence of Lyra geometry in present universe.
Paper Structure (12 sections, 55 equations, 10 figures)

This paper contains 12 sections, 55 equations, 10 figures.

Table of Contents

  1. Introduction
  2. Geometrical definitions
  3. Basic equations
  4. Solutions to the equations
  5. Case with constant potential
  6. Exponential potential
  7. Equation of motion within equation of state
  8. Perfect fluid case
  9. Exotic matter case
  10. Phantom matter case
  11. Quintessence model
  12. Conclusions

Figures (10)

  • Figure 1: Volume function V in case of dark energy.
  • Figure 2: Scalar field in case of dark energy.
  • Figure 3: Lyra's parameter $\beta$ in case of dark energy.
  • Figure 4: Lyra's parameter $\beta$ in case of trivial potential.
  • Figure 5: Lyra's parameter $\beta$ in case of exponential potential.
  • ...and 5 more figures