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Cosmological Evolution of a Quintom Model of Dark Energy
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Cosmological Evolution of a Quintom Model of Dark Energy
abstract
We investigate in this paper the cosmological evolution of a dark energy model with two scalar fields where one of the scalar has canonical kinetic energy and another scalar has negative kinetic energy term. For such a system with exponential potentials we find that during the evolution of the universe the equation of state $w$ changes from $w>-1$ to $w<-1$, which is consistent with the recent observations. A phase-plane analysis shows that the "phantom"-dominated scaling solution is the stable late-time attractor of this type of models.
Forward citations
Cited by 17 Pith papers
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Full DES data from SN+BAO+3x2pt yields w0=-0.84, wa=-0.44 with 2.2σ deviation from ΛCDM; adding DESI+CMB reaches 3.0σ while 3x2pt improves figure of merit by ~10%.
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Coupling a single fluid or scalar dark energy to the Nieh-Yan density removes its unstable perturbation, allowing a healthy quintom-B crossing and predicting gravitational-wave velocity birefringence.
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A scalar-vector-tensor dark-energy model crosses the phantom divide at low redshift with no ghost or Laplacian instabilities and growth signatures close to LCDM.
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Non-minimally coupled quintessence resolves the Planck-DESI Ω_m tension at >3σ while the effective equation of state stays above w=-1 and other tensions on neutrino mass and growth rate are relieved.
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Quintom Model Perturbations
A two-field quintom model reproduces w0waCDM perturbation features and is mildly favored over it in Bayesian fits to BAO, CMB, and SNIa data.
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Upper bounds on total neutrino mass in four phenomenological interacting dark energy models are derived from DESI DR2 BAO plus CMB and SNIa data, showing strong dependence on the interaction term form and statistical ...
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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 in the DESI Era: A Brief Review of Evidence, Beyond-$\Lambda$CDM Interpretations, and Tensions
DESI data hint that dark energy evolves (w0>−1, wa<0, phantom crossing) at 2.5–4.2σ, but the same expansion history can also be produced by interacting dark sectors, modified gravity, or non-cold dark matter.
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This review traces the history of dynamical dark energy, presents the no-go theorem against single-field crossing of w = -1, and surveys viable Quintom constructions including multi-field models and modified gravity i...
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A review arguing that current DESI/DES data favor Quintom-B dark energy, where the equation of state crosses w=-1 from below to above, with applications to bounces and CMB birefringence.
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Dark Energy in the DESI Era: A Brief Review of Evidence, Beyond-$\Lambda$CDM Interpretations, and Tensions
Review of DESI evidence for dynamical dark energy, its dependence on parametrization and datasets, and alternative beyond-LambdaCDM interpretations that may address cosmological tensions.
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A short review on Quintom dark energy theory
Quintom dark energy models permit the equation of state to cross w=-1, supporting bouncing cosmologies and CMB-based tests of dark energy nature.
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