Narrow Results

In this study, we investigated quintessence and tachyon field dark energy (DE) models for the inhomogeneous and anisotropic Ruban universe in $f(R,T)$ gravitation theory. We utilized the Hubble parameter in the field equations as $\frac{\beta }{\sqrt{t+\alpha }}$ for the solutions. Since DE candidates are classified according to the $\frac{p}{\rho }$ values of the EoS parameter $\omega$, we obtained the p and $\rho$ solutions for each DE candidate and analyzed the scalar field (SF) and scalar potential solution. We also talked about the model’s physical characteristics and parameters with the help of a various of graphics for redshift z and cosmic time t. Additionally, the statefinder parameters, which are essential tools for distinguishing various dark energy models, have been explored.

In this study, we obtain Einstein, Bergmann–Thomson (BT), Landau–Lifshitz (LL), Møller, Papapetrou (PP) and Tolman energy–momentum (EM) distributions for Ruban universe model in general relativity (GR) and teleparallel gravity (TG). We obtain same results for Einstein, Bergmann–Thomson and Landau–Lifshitz energy–momentum distributions in GR and TG. Also, we get same results for Einstein and Tolman energy–momentum distributions in GR. The Møller energy–momentum results are different in GR and TG. Also, using Ruban universe model, we obtain LRS Bianchi type I solutions and we get zero energy–momentum results for this universe model in GR and TG. These results of LRS Bianchi type I universe model agree with Aygün et al., Taşer et al., Doğru et al., Banerjee–Sen, Tryon and Xulu in different gravitation theories.