Cosmic Evolution in Self-Interacting Brans-Dicke Cosmology

Abstract

In this paper, we investigate the nature of self-interacting potential that can support the accelerated expansion of the universe as indicated by observational data. For this purpose, we consider the Bianchi type I (BI) universe model in the Brans-Dicke (BD) field scenario and use a power law for both the scalar field and the scale factor. It is found that the accelerated expansion of the universe can be discussed for a positive power law potential with negative values of the BD parameter. We also explore the evolution of energy density perturbations. This analysis indicates that the model allows growing modes for negative values of the BD parameter and $m>0$.

23 pages, 6 figures

References in corpus (5)

• Constraints on scalar-tensor models of dark energy from observational and local gravity tests
• Dynamics of Bianchi I Universe with Magnetized Anisotropic Dark Energy
• Dynamics of a magnetized Bianchi I universe with vacuum energy
• Role of Brans-Dicke Theory with or without self-interacting potential in cosmic acceleration
• Cosmology of Chameleons with Power-Law Couplings

Cited by in corpus (5)

• Dynamics of Axial Symmetric System in Self-Interacting Brans-Dicke Gravity
• Stellar Filaments in Self-Interacting Brans-Dicke Gravity
• Dynamics of Potentials in Bianchi Type Scalar-Tensor Cosmology
• Instability Analysis of Cylindrical Stellar Object in Brans-Dicke Gravity
• A New Approach to Flatness, Horizon and Late-time Accelerating Expansion Problems on the basis of Mach Principle