Beyond the equation of state: a second-order diagnostic for dynamical dark energy

Engineering notes

Engineering notes will be added by the Power for Solar editorial team.

Chinese explanation / 中文解读

中文解读待补充：本站会优先为光伏效率、钙钛矿太阳能电池、储能技术、太阳能热利用、BIPV、并网技术等高价值论文补充中文说明。

Original abstract

The first-order continuity equations determine the evolution of the energy densities but depend only on the instantaneous value of the dark-energy equation-of-state parameter. Differentiating these equations with respect to e-fold time introduces the term $ω'_{\rm DE}$ explicitly, providing a second-order probe of dark-energy dynamics. Consequently, while information about the evolution of the equation of state is encoded in the full dynamical solution, it is not explicit in the first-order continuity equations evaluated at a given epoch. The second-order formulation, therefore, provides a complementary description in which the local evolution of the equation of state appears directly through the curvature of the density trajectory. For a two-fluid interacting dark-sector model with linear coupling $Q_{AB}=αρ_AH$, the resulting second-order equation defines a curvature diagnostic, $\mathcal{C}=ρ_{DE}''/ρ_{DE}$, whose leading contribution, in the cosmological-constant limit, is $α^2$, while departures from $ω_{DE}=-1$ generate corrections through both $δω=1+ω_{DE}$ and the distinctive term $-3ω_{DE}'$. Unlike first-order analyses, this contribution is independent of the interaction strength and directly identifies dynamical dark energy. Applying the diagnostic to a CPL model with parameters consistent with DESI constraints, we recover $ω_{DE}'$ across the full redshift range for both weak and strong interactions. Noise propagation shows that the diagnostic is detectable with signal-to-noise ratio exceeding three for $σ_H/H\lesssim1.5\%$, while the degeneracy between $α$ and $ω_{DE}'$ remains negligible for $α\lesssim0.1$. In the non-interacting limit, the formalism naturally recovers the Caldwell--Linder thawing/freezing classification and extends it to interacting dark-energy models.

Links and sources

• Official / arXiv page
• PDF from original source

Comments