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Axion-Dilaton Destabilization and the Hubble Tension
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abstract
The discrepancy in measurements of the Hubble constant indicates new physics in dark energy, dark matter, or both. Drawing inspiration from string theory, where axions interact with the other moduli fields, including the dilaton, here we demonstrate that the dynamics of an interacting dilaton and axion naturally realizes the proposal of Early Dark Energy. In this setup, stabilization of the the dilaton is in part due to the axion, and in the early universe the dilaton contributes to dark energy. The combined axion-dilaton system is destabilized when the Hubble constant falls below the mass of the axion, triggering a phase of fast-roll evolution of the dilaton wherein its equation of state is $w=1$, and the early dark energy redshifts away as $a^{-6}$.
Forward citations
Cited by 6 Pith papers
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The $H_0$ world cup. II. A comprehensive competition between proposed Hubble tension solutions
Against a common 2025-26 dataset (Planck PR4, ACT DR6, SPT-3G, DESI DR2, Pantheon+), early dark energy and early modified gravity models win the H0 competition (~3σ residual tension), while radiation and late-time sol...
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Impact of ACT DR6 and DESI DR2 for Early Dark Energy and the Hubble tension
With ACT DR6 and DESI DR2, early dark energy still reconciles CMB and local Hubble measurements to about 2 sigma, and a profile likelihood shows prior-volume effects in Bayesian limits.
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Atomic Dark Matter, Interacting Dark Radiation, and the Hubble Tension
nuADaM, a model of atomic dark matter plus self-interacting dark radiation, improves cosmological fits and raises the inferred Hubble constant to about 72.6 km/s/Mpc.
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The Hubble Hunter's Guide
The least unlikely fixes to the Hubble tension raise the expansion rate in the decade before recombination, and these fixes generically leave oscillatory residuals in CMB spectra that resemble Planck's A_L and matter-...
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The $H_0$ World Cup. I. Summary of the baseline group stage results
In a systematic head-to-head analysis, early dark energy and early modified gravity models reduce the Hubble tension to about 3σ and are favored over ΛCDM, while radiation and late-time alternatives are not.
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The Hubble tension: A decade review
Pure early or late fixes to the Hubble tension are tightly constrained; remaining options are combined early-late interacting dark energy or new physics at the local-to-homogeneous transition.
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