Application of Shear-Induced Effects in f(R, T) Gravity for Modeling Cosmic Expansion

In the context of f(R, T) gravity, this work examines an anisotropic cosmological model taking into account a Bianchi Type-V spacetime with a dynamical matter-geometry coupling α(t) = αoa - m. We introduce a shear-dependent equation of state p = ωρ + ξσ2 and an anisotropy-evolving parameter ω = ωo + ω1(σ2/θ2), creating a feedback system between thermodynamic fluid characteristics and spacetime geometry. The analysis of energy conditions and the deceleration parameter demonstrate a transition from early deceleration to late-time acceleration, with a transition redshift consistent with observations and close agreement with the ΛCDM model. The model naturally explains cosmic acceleration without invoking a cosmological constant, while capturing early-universe anisotropy and late-time isotropy. The thermodynamic analysis also confirms that the proposed model is physically viable.