In this paper, we present a detailed investigation of two-fluid cosmological models formulated within the anisotropic Bianchi type I spacetime. The framework considers the universe to be filled with two distinct components: a standard barotropic fluid representing ordinary matter and radiation and a dark energy component introduced to account for the late-time accelerated expansion of the universe. Both interacting and non-interacting scenarios between the two fluids are examined, allowing us to assess how the exchange or absence of energy–momentum transfer influences the overall cosmological dynamics.

Einstein field equations are solved explicitly for each case, and the evolution of key physical and geometrical parameters—such as directional Hubble rates, expansion scalar, shear scalar, and the density parameters—is analyzed with reference to recent observational data. Our results indicate that the proposed models are most accurately described by quintessence-type dark energy, exhibiting behavior consistent with a dynamically evolving equation of state. A significant outcome of the analysis is that the total density parameter Ω remains invariant irrespective of whether the fluids interact, underscoring the robustness of the model.

Furthermore, the asymptotic behavior of the cosmological parameters aligns with the predictions of the standard ΛCDM model. In particular, we demonstrate that the deceleration parameter approaches q→ −1 and the jerk parameter tends to j(t)→1 as cosmic time t→∞, indicating a smooth approach toward a de Sitter phase. These outcomes suggest that the constructed two-fluid Bianchi type I models provide a viable theoretical framework compatible with current cosmological observations.