Saez-Ballester Theory Research Articles

Barrow holographic dark energy: reconstruction within Saez-Ballester theory in Kantowski-Sachs universe

Within the framework of the Saez-Ballester theory, the Barrow Holographic Dark Energy (BHDE) has been reconstructed. This reconstruction was carried out in a homogeneous and anisotropic KS universe that was filled with BHDE. The study examined both non-interacting and interacting scenarios, with the future event horizon serving as the IR cut-off. The analysis focused on the evolution of the equation of State parameter for both cases, as well as the trajectories of wDE−w′DE . Additionally, the study investigated the inflation of the Universe filled with BHDE by plotting the slow-roll parameters. Furthermore, a connection between the canonical scalar field and BHDE was explored, as the presence of a scalar field is often associated with inflation. Finally, the tensor-to-scalar ratio r is plotted which seems to lie within the acceptable range.

Five-Dimensional Strange Quark Bianchi Type-I Cosmological Model in The Framework of Saez Ballester Theory of Gravity

In this paper, we have constructed a five-dimensional Bianchi type I cosmological model with strange quark matter in the context of Saez-Ballester theory of gravity. We have discussed a five-dimensional cosmological model by using the special rule of variation for the Hubble parameter in the shape of H = Da-1 and the equation of state for strange quark matter. Two different models for n ≠ 0 and n = 0 have been discussed. Also, the accelerated expansion of the Universe has been discussed by using various physical parameters and its graphical representation.

LRS Bianchi Cosmological Model in Saez-Ballester Theory of Gravity with Time Varying Cosmological Constant

The present work deals with the study of a locally rotationally symmetric (LRS) Bianchi type-I cosmological model in the framework of a scalar-tensor theory of gravity formulated by Saez and Ballester with time varying cosmological constant. To obtain the explicit solutions of the Saez-Ballester field equations we assume the average scale factor to obey a power law expansion and the cosmological constant to be proportional to the energy density of the cosmic fluid. The dynamical behaviour of relevant cosmological parameters including the Hubble parameter, the deceleration parameter, the energy density, the pressure, the equation of state parameter, the cosmological constant, the shear scalar, the expansion scalar etc. are investigated graphically by examining their evolution versus the redshift parameter. The validation of the four energy conditions are also checked. We find the outcomes of the constructed model to be in good agreement with the recent observational data.

Studies on Bianchi type-III cosmological model with parametrization of deceleration parameter in a SBST theory

In this paper, we delve into the cosmological assessments concerning the deceleration parameter [Formula: see text] in the context of the Bianchi type-III cosmological model within the framework of the Saez–Ballester theory of gravitation. By postulating a proportional relationship between the shear scalar ([Formula: see text]) and the expansion scalar ([Formula: see text]), we derive solutions for the corresponding field equations. Additionally, we conduct an examination and evaluation of the model’s physical and kinematic parameters, including the jerk parameter and snap parameter, while also discussing the energy condition of the model. Through the depiction of graphical representations, we illustrate the variations of the cosmological parameters for specific sets of constants.

Cosmology of Tsallis and Kaniadakis holographic dark energy in Saez–Ballester theory and consideration of viscous van der Waals fluid

In the framework of Saez–Ballester (SB) theory, the current study proposes a reconstruction scheme for Tsallis and Kaniadakis holographic dark energy, particular cases of a more generalised Nojiri–Odintsov holographic dark energy (Nojiri and Odintsov, 2006; The European Physical Journal C, 2017, 77, pp.1-8.), with Hubble horizon and future event horizons serving as the universe’s respective trapping horizons. The Hubble parameter was rebuilt by placing a constraint on the metric potential inside the conservation equation. As a result, the holographic dark energy of Tsallis and Kaniadakis are recreated, and the cosmology and thermodynamics are examined. Lastly, an interacting van der Waals (VDW) coupled fluid model was examined in the context of bulk viscosity, and the behaviour of the equation of state (EoS) parameter was examined.

Anisotropic dark matter distribution in Saez–Ballester theory of gravitation

Anisotropic dark matter distribution in Saez–Ballester theory of gravitation

Bianchi Type-V space time with Tsallis holographic dark energy

In this paper, using the framework of Saez–Ballester theory, Bianchi Type-V metric Tsallis holographic dark energy models with interacting and non-interacting elements have been constructed. To obtain solutions for the model, we used correlation between metric potentials and varying deceleration parameters. There is additional discussion of the models’ physical characteristics and behavior.

Particle creation and bulk viscosity in Bianchi-I universe in Saez–Ballester theory with different deceleration parameters

Particle creation and bulk viscosity in Bianchi-I universe in Saez–Ballester theory with different deceleration parameters

Kantowski–Sachs Barrow holographic dark energy model in Saez–Ballester theory of gravitation

In this paper, we have studied a spatially homogeneous and anisotropic Kantowski–Sachs universe in the presence of Barrow Holographic Dark Energy in the background of Saez–Ballester scalar–tensor theory of gravitation. To find the exact solution of the SB field equations, we have assumed that the shear scalar is directly proportional to expansion scalar. This assumption leads to relation between metric potentials of the models. We have discussed non-interacting and interacting cosmological models. Moreover, we have discussed several cosmological parameters such as energy densities of DM and DE (ρm &ρb), deceleration (q), equation of state (ωb) and skewness (α) parameters, squared sound speed (vs2), ωb−ωb′ plane statefinders and Om-diagnostics parameters through graphical representation for both the interacting models. Also, we have observed that the current values of deceleration and EoS parameters of our constructed models are coincide with the recent observational data.

The study of accelerating DE models in Saez–Ballester theory of gravitation

The study of accelerating DE models in Saez–Ballester theory of gravitation

Five Dimensional FRW Radiating Cosmological Model in Presence of Bulk Viscous Fluid in Scalar Tensor Theory of Gravitation

In this paper using the Saez-Ballester scalar-tensor theory of gravitation, we examined a 5-dimensional FRW cosmic space-time in a source of bulk viscous fluid in the article. To examine determinate solutions of the field equations, we used a power law between a scalar field and the universe's scale factor. Our research considers radiating flat, closed, and open models. The physical and kinematical properties of the models were explored in each scenario. In this study, we show that our model expands and is free of initial singularities, as well as that our models decelerate in a conventional manner.
 HIGHLIGHTS
 
 Using the Saez-Ballester theory and a 5-dimensional FRW space-time as a source of bulk viscous fluid, we have obtained cosmological models that can be assumed to be equivalent radiating models in closed, open, and flat space-times
 We have obtained models that are expanding and free of initial singularity
 We used a power law between a scalar field and the universe's scale factor

Five Dimensional Bianchi Type-I Anisotropic Cloud String Cosmological Model With Electromagnetic Field in Saez-Ballester Theory

Within the context of Saez-Ballester theory, we explored the interaction of a five-dimensional Bianchi type-I anisotropic cloud string cosmological model Universe with an electromagnetic field. With an electromagnetic field, the energy momentum tensor is assumed to be the sum of the rest energy density and string tension density in this paper. We use the average scale factor as an integrating function of time to get exact answers to Saez-Ballester equations. The dynamics and importance of the model’s many physical parameters are also examined.

Vacuum Energy in Saez-Ballester Theory and Stabilization of Extra Dimensions

In this work, we study a spherically symmetric metric in 5D within the framework of Saez-Ballester Theory, where minimal dark energy-matter interaction occurs. We predict that the expanding isotropic universe will be progressively DE dominated. We estimate few values of the deceleration parameter, very close to the recently predicted values. We obtain the value of the DE EoS parameter as ω=−1. Additionally, we measure the value of the overall density parameter as Ω=0.97(≈1), in line with the notion of a close to or nearly (not exactly) flat universe. We predict that the model universe starts with the Big-Bang and ends at the Big Freeze singularity. In general, we cannot find conditions for stabilization of extra dimensions in general relativity, and all dimensions want to be dynamical. Here, we present two possible conditions to solve this stabilization problem in general relativity.

Bianchi Type-I Anisotropic Universe with Metric Potential in Saez-Ballester Theory of Gravitation

Bianchi Type-I cosmological model in the presence of Saez-Ballester theory gravitation is studied. An exact solution of the field equation is given by considering the cosmological model yield a metric potential included with a real number. The relation between the deceleration parameter and Hubble parameter and average scale factor is used in that cosmological model. The effect of the viscosity on the entropy of the universe is utilized by energy momentum tensor with bulk viscous terms in a conservative manner. We obtained a formula for calculating the entropy of the universe in terms of viscosity and used it to compare to the study. Also, various physical and kinematical properties have been discussed.

FRW cosmological models in presence of a perfect fluid within the framework of Saez-Ballester theory in five dimensional space time

In the framework of Saez-Ballester scalar-tensor theory of gravity, five-dimensional FRW space-time is considered in the presence of perfect fluid. We employed a power law between the scalar field and the universe's scale factor to get a definite solution to the field equations. Models that radiate flat, closed and open universe are shown. The model's physical features are also discussed.

Cosmological models of generalized ghost pilgrim dark energy (GGPDE) in the gravitation theory of Saez–Ballester

In this paper, we study the mechanism of the cosmic model in the presence of generalized ghost pilgrim dark energy (GGPDE) and matter in locally rotationally symmetric (LRS) Bianchi type-I space-time by the utilization of new holographic DE in Saez–Ballester theory. Here, we discuss all the data for three scenarios, the first is supernovae type-Ia union data, the second is SN Ia data in combination with baryon acoustic oscillation and cosmic microwave background observations and the third is a combination with observational Hubble data and joint light-curve analysis observations. From this, we get a model of our universe, where transit state exists from deceleration to acceleration phase. Here, we have observed that the results yielded by cosmological parameters like [Formula: see text] (energy density), equation of state [Formula: see text], squared speed of sound [Formula: see text] and [Formula: see text]–[Formula: see text] are compatible with the recent observations. The [Formula: see text]–[Formula: see text] trajectories lie in both thawing and freezing regions and the correspondence of the quintessence field with GGPDE is also discussed. Some physical aspects of the GGPDE models are mainly highlighted.

Higher dimensional phantom dark energy model ending at a de-Sitter phase

In this work, using a spherically symmetric metric, we investigate a minimally interacting holographic dark energy model within the framework of the Saez-Ballester Theory. We predict that the dark energy component dominating the universe is of phantom type, which will lead the model universe to cosmic doomsday (big rip singularity). As the big rip singularity and holographic dark energy are incompatible with each other, we employ a higher dimensional scenario so that the cosmic doomsday is replaced by a de-Sitter phase. The model expands with a slow and uniform change of size during the early evolution, whereas the change becomes faster and faster, agreeing with the present observation of the accelerated expansion. The present values of the Hubble parameter and the dark energy EoS parameter are found to be H=67 and λ=−1.00011, which agree with the respective values H0=67.36±0.54kms−1Mpc−1and λ=−1.03±0.03 of the most recent Planck 2018 result.

Kantowski–Sachs viscous Ricci dark energy model in Saez–Ballester theory of gravitation

Kantowski–Sachs viscous Ricci dark energy model in Saez–Ballester theory of gravitation

Axially symmetric domain walls cosmology in Saez-Ballester theory of gravitation

In this present research paper, we considered cosmological model in Saez-Ballester [Phys. LettA 113, 467, 1985] theory of gravitation with stiff matter, thick domain walls. Some physical and geometrical aspects of the models have also been discussed

Kaluza-Klein FRW dark energy models in Saez-Ballester theory of gravitation

This article is concerned with the investigation of dynamical behaviour of Kaluza-Klein(KK) FRW type dark energy cosmological models in the framework of a scalar-tensor theory of gravitation formulated by Saez and Ballester (Phys. Lett. A113,467:1986). Three cosmological models, in this theory, are presented by solving the field equations using (i) hybrid expansion law given by Pradhan et al. (Ind.J.Phys.89,5032015), (ii)varying deceleration parameter proposed by Mishra et al.(Int. J. Theor. Phy.52, 2546: 2013) and(iii)linearly varying deceleration parameter defined by Akarsu and Dereli (Int. J. Theor. Phys. 51, 612: 2012). We have evaluated the dynamical parameters for each of the models, namely, the equation of state (EoS) parameter, the deceleration parameter, statefinder parameter and total energy density parameter of dark energy. We have also found the scalar field in the models. We have discussed the dynamical behavior of the parameters through graphical representation with special reference to Planck Collaboration data. It is observed that our models describe accelerated expansion of the universe and our theoretical results are, reasonably, in good agreement with the observational data.