Quintessence black holes produce observer-dependent shadow angular sizes, with infalling observers seeing smaller shadows than static ones, yielding stronger equation-of-state constraints from M87* observations.
Quintessence: A Review
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abstract
Quintessence is a canonical scalar field introduced to explain the late-time cosmic acceleration. The cosmological dynamics of quintessence is reviewed, paying particular attention to the evolution of the dark energy equation of state w. For the field potentials having tracking and thawing properties, the evolution of w can be known analytically in terms of a few model parameters. Using the analytic expression of w, we constrain quintessence models from the observations of supernovae type Ia, cosmic microwave background, and baryon acoustic oscillations. The tracking freezing models are hardly distinguishable from the LCDM model, whereas in thawing models the today's field equation of state is constrained to be w_0<-0.7 (95 % CL). We also derive an analytic formula for the growth rate of matter density perturbations in dynamical dark energy models, which allows a possibility to put further bounds on w from the measurement of redshift-space distortions in the galaxy power spectrum. Finally we review particle physics models of quintessence- such as those motivated by supersymmetric theories. The field potentials of thawing models based on a pseudo-Nambu-Goldstone boson or on extended supergravity theories have a nice property that a tiny mass of quintessence can be protected against radiative corrections.
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An analytic bound on axion parameters in thawing quintessence is derived independently of initial conditions and used with cosmological observations plus quantum gravity constraints to exclude large regions of axion dark energy parameter space.
A Hubble-scale domain wall quintessence model produces anisotropic expansion but is tightly constrained by Planck CMB quadrupole limits and supernova data to a negligible contribution, favoring standard LambdaCDM.
Extends the equivalence of second-order EOM to first-order Bogomolnyi equations from single real/complex scalars to arbitrary real multi-component scalar fields without fixing the Lagrangian.
Extended analysis of DESI DR2 data confirms robust evidence for dynamical dark energy with phantom crossing preference, stable under parametric and non-parametric modeling.
String theory imposes constraints on dark energy but permits various construction attempts for de Sitter vacua and single-field exponential quintessence models despite obstructions.
citing papers explorer
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Shadows of quintessence black holes: spherical accretion, photon trajectories, and geodesic observers
Quintessence black holes produce observer-dependent shadow angular sizes, with infalling observers seeing smaller shadows than static ones, yielding stronger equation-of-state constraints from M87* observations.
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Bounding axion dark energy
An analytic bound on axion parameters in thawing quintessence is derived independently of initial conditions and used with cosmological observations plus quantum gravity constraints to exclude large regions of axion dark energy parameter space.
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Domain-wall Quintessence
A Hubble-scale domain wall quintessence model produces anisotropic expansion but is tightly constrained by Planck CMB quadrupole limits and supernova data to a negligible contribution, favoring standard LambdaCDM.
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Multi-component scalar fields and the complete factorization of its equations of motion
Extends the equivalence of second-order EOM to first-order Bogomolnyi equations from single real/complex scalars to arbitrary real multi-component scalar fields without fixing the Lagrangian.
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Extended Dark Energy analysis using DESI DR2 BAO measurements
Extended analysis of DESI DR2 data confirms robust evidence for dynamical dark energy with phantom crossing preference, stable under parametric and non-parametric modeling.
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Dark energy from string theory: an introductory review
String theory imposes constraints on dark energy but permits various construction attempts for de Sitter vacua and single-field exponential quintessence models despite obstructions.