Inflationary Cosmological Model of Bianchi Type VI0 with Exponential Potential

LRS Bianchi Type VI₀ inflationary spacetime under the impact of the effective potential V(?) = ? − l?, l > 0, where ? Higgs field is denoted by ?, has been determined in the current study. It is advised to use the average scale factor (R³) = B²A = ?l? to get the exact solution. Under certain conditions, the model becomes isotropic and shear- free. Also, the model does not show singularity at initially. The effective potential's evolution indicates that the model is consistent with an inflationary scenario in which the universe experiences a rapid expansion in its early stages. Throughout its development, the model displays anisotropic properties because the shear to expansion ratio s/q is nonzero. This study indicates the significance of anisotropic inflationary models for solving basic cosmological challenges like the flatness and horizon problems. The deceleration parameter q plays a crucial role in determining whether the universe undergoes accelerated or decelerated expansion. We have used hubble parameter, expansion scalar and shear scalar to discuss the model's kinematic and physical behavior. The results underline how crucial inflationary scenarios are for describing the observed homogeneity and large-scale structure of the current cosmos.