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Can interacting dark energy with dynamical coupling resolve the Hubble tension
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abstract
The $H_0$ tension between low- and high- redshift measurements is definitely a serious issue faced by current cosmologists since it ranges from 4$\sigma$ to 6$\sigma$. To relieve this tension, in this paper we propose a new interacting dark energy model with time varying coupling parameter by parameterizing the densities of dark matter and dark energy, this parametric approach for interacting dark sectors are inspired by our previous work concerning the coupled generalized three-form dark energy model in which dark matter and dark energy behave like two uncoupled dark sectors with effective equation of state when the three-form $|\kappa X|\gg1$, for this reason, we reconstruct coupled generalized three-form dark energy from such parametric model under the condition $|\kappa X_0|\gg1$. In the end, we place constraints on three parametric models in light of the Planck 2018 cosmic microwave background (CMB) distance priors, baryon acoustic oscillations (BAO) data and the Pantheon compilation of Type Ia supernovae (SN Ia) data by assuming the parameter $k$ as 0,5,10 respectively. The fitting results show that, for all the observational data sets, the parametric models with $k=0,5,10$ relieve the Hubble tension with the latest local determinations of the Hubble constant from ${\rm SH_0ES}$ team, i.e. the so called R22, to 2.3 $\sigma$, 1.9 $\sigma$ and 1.3 $\sigma$ with $\chi_{\rm min}^2=10.43,10.47,10.48$ respectively, revealing that $k$ is positive correlated to the Hubble constant.
Forward citations
Cited by 7 Pith papers
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Early- and late-time constraints on Wald-Gauss-Bonnet topological dark energy and implications for the $H_0$ and $S_8$ tensions
A joint CMB, BAO, and supernova fit mildly prefers a non-zero Wald-Gauss-Bonnet dark-energy term (~3σ with SH0ES included), raising H0 from 68.5 to 69.8 km/s/Mpc and easing the Hubble tension by ~0.9σ at the cost of a...
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BAO miscalibration cannot rescue late-time solutions to the Hubble tension
Even after rescaling BAO data to prefer H0≈73 km/s/Mpc, none of six tested late-time dark-energy models can resolve the Hubble tension once unanchored SNeIa and CMB geometry are included.
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Robust Preference for Dark Sector Interactions
Interacting dark matter–dark energy models fit DESI BAO and CMB data as well as evolving-dark-energy (CPL) models, with a coupling preference that persists under DES-Dovekie supernova recalibration.
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Model-independent late-universe measurements of $H_0$ and $\Omega_K$ with the parametrization based on cosmic age-improved inverse distance ladder
A cosmic-age-based inverse distance ladder with DESI DR2, DESY5, SGL, CC and GRB data gives H0=71.59±0.94 km/s/Mpc and ΩK=0.001±0.038.
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Neutrino mass constraints in the Schwarzschild-de Sitter black-hole dark energy model with ACT DR6 and DESI DR2 data
SdSDE dark energy yields a ~0.16–0.21 eV positive neutrino-mass preference with DESI+ACT data, but χ² strongly favors extended ΛCDM and the shift is likely compensation.
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Alleviating the $H_0$ tension through the interacting dark energy model from quantum gravitational field theory in light of DESI DR2
With DESI DR2 BAO plus CMB and a SH0ES prior, the two-parameter eeΛCDM model gives δΛ=-0.41±0.14 and H0=71.9±1.0, easing the Hubble tension to 0.8σ, but SN datasets erase the signal.
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Dark Energy Is Not That Into You: Variable Couplings after DESI DR2 BAO
With DESI DR2 data, one interacting dark sector model with a time-dependent coupling shows a nonzero coupling at more than 95% CL, but Bayesian evidence still favors Lambda-CDM.
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