A density-responsive scalar-field framework for singularity regularization and dynamical dark energy

Abstract

We present a covariant scalar-field framework that unifies the space-time singularity regularization with dynamical dark energy. The theory extends general relativity by introducing a scalar field $\Phi$ whose potential couples to the Lorentz-invariant quantity $X \equiv u_{\alpha} u_{\beta} T^{\alpha\beta}_{\mathrm{matter}}$, ensuring manifest covariance. The resulting density-responsive scalar energy $\rho_\Phi$ exhibits dual behavior: (i) in high-density regimes, it saturates at $\rho_\Phi \leq AM_P^4/2$, providing a Planck-scale upper bound on the total energy density that regularizes classical singularities; (ii) in low-density regimes, it approaches a constant $\rho_\Phi \to AM_U^4$, driving cosmic acceleration as dynamical dark energy. A natural renormalization group evolution with an anomalous dimension $\gamma \approx 0.501$ connects the Planck scale to the meV dark energy scale without fine-tuning. The model makes distinctive, testable predictions: $w_0 \approx -0.99$ and $w_a \approx +0.03$, where the positive $w_a$ distinguishes it from $\Lambda$CDM and standard quintessence models. Despite the novel interaction terms, the fifth forces are suppressed by $\beta_{\rm eff} \propto 1/\rho_m^2$, yielding factors below $10^{-58}$ in laboratory environments, and ensuring compatibility with all precision gravity tests. This framework demonstrates how a single quantum field theory mechanism can simultaneously address UV singularities and IR dark energy, providing concrete predictions for future Stage-IV cosmological surveys.