We also discuss many other issues of the MEF model. In the framework of the MTIG, the mechanism of phase transitions and the description of multiphase behavior of the cosmological scenario are proposed. Here, we use this idea and develop a modified dynamical model of cosmology based on imposing Neumann boundary condition on cosmological perturbation equations. This work is the extension of author’s research, where the modified theory of induced gravity (MTIG) is proposed. Cosmology Group Department of Mathematics and Applied Mathematics University of Cape Town, Rondebosch 7701, Cape Town, South Africa September 2, 2008 Abstract The aim of this set of lectures is a systematic presentation of a 1 + 3 covariant approach to studying the geometry, dynamics, and observational properties of relativistic cosmological models. A modified version of the Ozer and Taha nonsingular cosmologicla model is presented on the assumption that the universe's radius is complex if it is regarded as empty, but it …
The main ``modification'' that underpins this work is to consider the principle of greatest action, not least, but cosmological energy functions do not appear. Interesting features of generalisations to other teleparallel models, spatially curved backgrounds, and rotated tetrads are pointed out. The modified entropic force (MEF) model is in fact a modified gravity model, and the universe can be accelerated without dark energy. We will review recent developments in models of modified gravity and explain why the realisation of a screening mech-anism is important in these models. In addition, a modified Hubble parameter is derived due to the presence of the new term.
Full sets of linear perturbation equations are accurately derived and analysed at the relevant limits. Subsequently we propose the model as a remedy to cosmological anomalies, namely the tension between observed and predicted tensor-to-scalar mode ratios in the cosmic microwave background and the different values of the Hubble constant measured at different cosmological scales.
Non-Minimal Cosmological Model in Modified Yang-Mills Theory Shchigolev, V. K.; Orekhova, G. N. Abstract. The modified cosmological model (MCM) has been an active research program since 2009 and here we summarize the highlights while providing background and insights as they demonstrate mathematical merit. Rev. Cosmological equations were recently derived by Padmanabhan from the expansion of cosmic space due to the difference between the degrees of freedom on the surface and in the bulk in a region of space. The Friedmann-Robertson-Walker (FRW) model with dynamical Dark Energy (DE) in the form of modified Chaplygin gas (MCG) has been investigated. (Phys. Because the term depends on the prevailing consensus, the meaning of the term changes over time. Then, it is shown that a new term appears in the equation of motion which leads to a modified Poisson equation. Cosmological perturbations are considered in f(T) and in scalar-torsion f()T teleparallel models of gravity.
He observed that the power-law model depends upon its parameters is while the exponential model acts like a cosmological model at high redshift, and here (with our viscous F(T) gravity), we studied the universe at low/high redshift z. Download Citation | Cosmological Models in Modified f(R) Gravity Theories | The actual accelerated expansion of the universe continues being a mystery in physics. The theory describes two systems (stages): Einstein (ES) and “restructuring” (RS). These difficulties sharpened with the discovery of CMB anisotropy by the Cosmic Background Explorer in 1992, and several modified CDM models, including ΛCDM and mixed cold and hot dark matter, came under active consideration through the mid-1990s. In present paper, we have investigated Bianchi type-III cosmological model in modified [equation] theory of gravity as proposed by Harko et al. In this paper, we consider a model of non-minimal modified Yang-Mills (Y-M) theory in the Friedmann-Robertson-Walker (FRW) cosmology, in which the Y-M field couples to the scalar curvature through a function of its first invariant. The present paper deals with a spatially homogenous Bianchi Type- I massive string cosmological model with bulk viscosity and decaying vacuum energy density. The main ``modification'' that underpins this work is to consider the principle of greatest action, not least, but cosmological energy functions do not appear.
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