In this paper, we have investigated some features of anisotropic accelerating Bianchi type-I cosmological model in the presence of two non-interacting fluids, i.e. one usual string and other dark energy fluid towards the gravitational field equations for the linear form of $f(T)$ gravity, where \textit{T }be the torsion. To achieve a physically realistic solution of the field equations, we have considered an exact matter dominated volumetric power law expansion. The aspects of derived model are discussed with the help of solution and make the model at late times turn out to be flat Universe. Also, observed that the model has initially non-singular and stable while for whole expansion it is unstable. At an initial expansion $0.01\le t\le 0.05$ when the Universe start to expand to infinite expansion $t>1.73$ (break away from for small interval of cosmic time $0.06\le t\le 1.73$), there is a matter dominated era while for $0.06\le t\le 1.73$ it approaches the quintessence region. Also, the string exists in the early universe which is in agreement with constraints of CMBR data but with the expansion the string phase of the Universe disappears, i.e. we have an anisotropic fluid of particles.
A New Class of Bianchi Type-I Cosmological Models in Scalar-Tensor Theory of Gravitation and Late Time Acceleration
在Saez和Ballester（Phys. Lett. 113：467，1986）进行了研究。要占上风的确定性解决方案，我们选择不同的比例因子，产生依赖于时间的减速参数（DP）表示模型，产生宇宙从早期的减速阶段到最近的加速阶段的过渡。得到了三种不同的物理可行的宇宙模型，它们的各向异性解可能进入各向同性暴胀时代。精确求解了修正的爱因斯坦场方程，发现模型与最近的观测结果很好地一致。文中还讨论了模型的一些物理和几何性质。
Dark Energy Model in Anisotropic Bianchi Type-III Space-Time with Variable EoS Parameter
研究了各向异性Bianchi III型时空中一个新的变状态方程参数的暗能量模型。为了得到确定性模型，我们认为模型中的展开式$θ$与剪切张量$σ^{j}_~i$的本征值$σ^{2}_{~2}$成正比。EoS参数$ω$被发现是时间依赖的，它的现有范围与最近的观测SNe Ia数据（Knop et al. 2003）和SNe Ia数据与CMBR各向异性和星系聚类统计（Tegmark et al. 2004）是一致的。有人认为，解释宇宙加速膨胀的暗能量可能是由于在依赖于时间的背景下对EoS真空能量的贡献而产生的。本文还讨论了暗能量模型的一些物理问题。
