Observations of the universe's expansion history, particularly using Type Ia supernovae and baryon acoustic oscillations, indicate that the cosmic expansion is not only accelerating but is asymptotically approaching an exponential growth rate consistent with a de Sitter phase. In the Lambda-CDM model, this behavior is mathematically described by the dominance of a constant vacuum energy density (Lambda) as matter dilutes. However, the physical origin of this specific late-time behavior—why the universe transitions to an exponential trend at this specific epoch rather than earlier or later—remains unexplained, often referred to as the cosmic coincidence problem, and lacks a dynamical mechanism beyond the static value of the cosmological constant (Riess et al. 1998; Perlmutter et al. 1999).