In this work, the generalized Quantum Chromodynamics (QCD) ghost model of dark energy in the framework of Einstein gravity is investigated. For this purpose, we use the squared sound speed $ v_{s}^{2}$ whose sign determines the stability of the model. At first, the non-interacting ghost dark energy in a Bianchi type-I (BI) background is discussed. Then the equation-of-state parameter, $ \omega_D=p_{D}/\rho_{D}$ , the deceleration parameter, and the evolution equation of the generalized ghost dark energy are obtained. It is shown that the equation-of-state parameter of the ghost dark energy can cross the phantom line ( $ \omega=-1$ in some range of the parameter spaces. Then, this investigation was extended to the general scheme for modified $ f(R,T)$ gravity reconstruction from a realistic case in an anisotropic Bianchi type-I cosmology, using the dark matter and ghost dark energy. Special attention is taken into account for the case in which the function f is given by $ f(R,T)=f_{1}(R) +f_{2}(T)$ . We consider a specific model which permits the standard continuity equation in this modified theory. Besides $ \Omega_{\Lambda}$ and $ \Omega$ in standard Einstein cosmology, another density parameter, $ \Omega_{\sigma}$ , is expected by the anisotropy. This theory implies that if $ \Omega_{\sigma}$ is zero then it yields the FRW universe model. Interestingly enough, we find that the corresponding f (R, T) gravity of the ghost DE model can behave like phantom or quintessence of the selected models which describe the accelerated expansion of the universe.
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Dec 19, 2023
Sibel Korunur 
Open Access