Spatial Phonons: A Phenomenological Viscous Dark Energy Model for DESI

Spatial Phonons: A Phenomenological Viscous Dark Energy Model for DESI
Muhammad Ghulam Khuwajah Khan
arXiv:2512.00056v2 Announce Type: replace
Abstract: We explore a phenomenological model of dark energy in which space is treated as an elastic brane with uniform tension $T_s$ supporting a longitudinal phonon fluid. The brane tension gives a residual geometric contribution to the vacuum energy, while the phonon sector is described by three scalar fields $phi^I$ and an invariant $b = sqrt{det B_{IJ}}$ entering an effective action $F(b)$. At the background level this reproduces a perfect fluid with energy density, pressure and bulk modulus set by two dimensionless parameters $varepsilon$ and $kappa$. These parameters fix the enthalpy and bulk modulus in units of the space tension and determine the phonon sound speed through $c_s^2 = kappa/varepsilon$. Dissipative effects are modeled by a bulk viscous pressure obeying a Maxwell type relaxation law with a characteristic time scale $tau(H)$ that depends on the Hubble rate. Motivated by a Boltzmann suppressed scattering rate at a mass-gap scale $H_star$, we adopt a simple ansatz for $Htau(H)$ and obtain a compact expression for the effective dark energy equation of state $w_{rm eff}(H)$. The viscous correction is transient, is most active around $H sim H_star$ and drives a temporary phantom deviation. At the same time, we also show that $w_{rm eff}$ approaches $-1 + varepsilon$ at very early and very late times. Using a flat $Lambda$CDM background for $H(z)$, we scan the parameter space and identify a region with $kappa simeq varepsilon simeq 1/3$ and $H_star/H_0 simeq 2.1$. This choice gives an ultralight phonon with sound speed close to the causal limit and a viscous dark energy history $w_{rm eff}(z)$ that closely tracks a DESI motivated Chevallier-Polarski-Linder parametrization over the redshift range most relevant for the DESI BAO measurements.arXiv:2512.00056v2 Announce Type: replace
Abstract: We explore a phenomenological model of dark energy in which space is treated as an elastic brane with uniform tension $T_s$ supporting a longitudinal phonon fluid. The brane tension gives a residual geometric contribution to the vacuum energy, while the phonon sector is described by three scalar fields $phi^I$ and an invariant $b = sqrt{det B_{IJ}}$ entering an effective action $F(b)$. At the background level this reproduces a perfect fluid with energy density, pressure and bulk modulus set by two dimensionless parameters $varepsilon$ and $kappa$. These parameters fix the enthalpy and bulk modulus in units of the space tension and determine the phonon sound speed through $c_s^2 = kappa/varepsilon$. Dissipative effects are modeled by a bulk viscous pressure obeying a Maxwell type relaxation law with a characteristic time scale $tau(H)$ that depends on the Hubble rate. Motivated by a Boltzmann suppressed scattering rate at a mass-gap scale $H_star$, we adopt a simple ansatz for $Htau(H)$ and obtain a compact expression for the effective dark energy equation of state $w_{rm eff}(H)$. The viscous correction is transient, is most active around $H sim H_star$ and drives a temporary phantom deviation. At the same time, we also show that $w_{rm eff}$ approaches $-1 + varepsilon$ at very early and very late times. Using a flat $Lambda$CDM background for $H(z)$, we scan the parameter space and identify a region with $kappa simeq varepsilon simeq 1/3$ and $H_star/H_0 simeq 2.1$. This choice gives an ultralight phonon with sound speed close to the causal limit and a viscous dark energy history $w_{rm eff}(z)$ that closely tracks a DESI motivated Chevallier-Polarski-Linder parametrization over the redshift range most relevant for the DESI BAO measurements.