Abstract
Locally rotationally symmetric (LRS) Bianchi type-I dark energy cosmological model with variable equation of state (EoS) parameter in (Nordtvedt 1970) general scalar tensor theory of gravitation with the help of a special case proposed by (Schwinger 1970) is obtained. It is observed that these anisotropic and isotropic dark energy cosmological models always represent an accelerated universe and are consistent with the recent observations of type-Ia supernovae. Some important features of the models, thus obtained, have been discussed.
Highlights
Nordtvedt [1] proposed a general class of scalar tensor gravitational theories in which the parameter ω of the Brans-Dicke (BD) theory is allowed to be an arbitrary function of the scalar field (ω → ω(φ))
We will study Locally rotationally symmetric (LRS) Bianchi type-I dark energy cosmological models in the Nordtvedt [1] general scalar tensor theory with the help of a special case proposed by Schwinger [27], that is, 3 + 2ω(φ) = (1/λφ), where λ is a constant
We have presented a spatially homogeneous LRS Bianchi type-I anisotropic as well as isotropic dark energy cosmological models in the Nordtvedt [1] general scalar tensor theory of gravitation with the help of a special case proposed by Schwinger [27]
Summary
Nordtvedt [1] proposed a general class of scalar tensor gravitational theories in which the parameter ω of the Brans-Dicke (BD) theory is allowed to be an arbitrary (positive definite) function of the scalar field (ω → ω(φ)). There has been considerable interest in cosmological models with dark energy in general relativity because of the fact that our universe is currently undergoing an accelerated expansion which has been confirmed by a host of observations, such as type Ia supernovae (Reiss et al [13]; Perlmutter et al [14]; and Tegmark et al [15]). We will study LRS Bianchi type-I dark energy cosmological models in the Nordtvedt [1] general scalar tensor theory with the help of a special case proposed by Schwinger [27], that is, 3 + 2ω(φ) = (1/λφ), where λ is a constant
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