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The Dynamics of Quintessence, The Quintessence of Dynamics
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Quintessence theories for cosmic acceleration imbue dark energy with a non-trivial dynamics that offers hope in distinguishing the physical origin of the component. We review quintessence models with an emphasis on this dynamics and discuss classifications of the different physical behaviors. The pros and cons of various parameterizations are examined as well as the extension from scalar fields to other modifications of the Friedmann expansion equation. New results on the ability of cosmological data to distinguish among and between thawing and freezing fields are presented.
Forward citations
Cited by 9 Pith papers
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Breaking the Dark Sector Degeneracy with Nonparametric Expansion--Growth Reconstruction
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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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Physical vs phantom dark energy after DESI: thawing quintessence in a curved background
Curved thawing quintessence models fit DESI DR2 BAO, CMB, and Pantheon+ data as well as the flat w0-wa parametrization, so phantom crossing is model-dependent rather than required.
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The Goldstone Awakens: Unimodular dark energy in scale-invariant $R^2$ gravity
In a scale-invariant R² + unimodular-gravity model, the Goldstone boson of scale symmetry becomes thawing dark energy, with its equation of state fixed by the same coupling that sets the inflationary spectral tilt.
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Fermi scale from quantum gravity scaling solution
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Hamilton-Jacobi analysis of slow-roll inflation with non-Bekenstein-Hawking entropies yields fitted entropy parameters (δ≈1.1-1.2, α∼10^{-14}, K∼10^{-17}) consistent with ns and r data.
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