The authors reformulate the equations of motion for AdS_D × I solutions in axio-dilaton gravity as a first-order autonomous dynamical system, identify fixed points and analytic solutions for arbitrary D including in type IIB, and discuss numerical flows in massive IIA.
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Exponential potentials and cosmological scaling solutions
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abstract
We present a phase-plane analysis of cosmologies containing a barotropic fluid with equation of state $p_\gamma = (\gamma-1) \rho_\gamma$, plus a scalar field $\phi$ with an exponential potential $V \propto \exp(-\lambda \kappa \phi)$ where $\kappa^2 = 8\pi G$. In addition to the well-known inflationary solutions for $\lambda^2 < 2$, there exist scaling solutions when $\lambda^2 > 3\gamma$ in which the scalar field energy density tracks that of the barotropic fluid (which for example might be radiation or dust). We show that the scaling solutions are the unique late-time attractors whenever they exist. The fluid-dominated solutions, where $V(\phi)/\rho_\gamma \to 0$ at late times, are always unstable (except for the cosmological constant case $\gamma = 0$). The relative energy density of the fluid and scalar field depends on the steepness of the exponential potential, which is constrained by nucleosynthesis to $\lambda^2 > 20$. We show that standard inflation models are unable to solve this `relic density' problem.
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Any unified early and late dark energy scenario with a single tracking scalar field requires a potential with three distinct slopes arranged in a steep-steeper-shallow hierarchy.
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Analytical formulae for power spectrum peaks in constant-roll inflation enable parameter reconstruction from peak features and smoothed approximations for induced gravitational wave estimates.
Proposes phase-resolved invariant path-length criteria and a master formula for lower bound on ε_ek in ekpyrotic cosmologies, using BKL suppression and conversion windows as constraints.
Scalar and tensor perturbations in Jordan-frame scalar-tensor gravity admit an exact linear-order Eckart effective-fluid description, with gravitational-wave damping governed by the scalar sector's transverse-traceless anisotropic stress.
Improved end-of-inflation dynamics shift the Starobinsky model's predicted spectral index n_s by up to 1.2×10^{-3} within the allowed reheating range.
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.
FRW scalar-field cosmologies with fluid and curvature are organized by five parameter loci with explicit reduced normal forms, and a new arctan-slope variable extends the atlas to quadratic potentials.
Exponential quintessence with an assumed kination epoch relaxes the dark energy fine-tuning problem by dozens of orders of magnitude relative to a cosmological constant.
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.
For an exponential quintessence potential, an analytic formula links the current equation-of-state w_φ0 to the potential slope λ while enforcing prior radiation and matter domination, yielding the bound λ < 1.94 at Ω_φ0 = 0.685.
Observational constraints on teleparallel cubic Galileon cosmologies with quadratic and exponential potentials show viability for late-time acceleration, with the fixed b1 quadratic case competitive under AIC but not BIC.
In a 5D open FRW model, negative curvature sustains tracker-like radion evolution that enables dynamical compactification via Casimir stabilization before 4D inflation dilutes curvature remnants.
Reconstruction of EFT background functions from cosmic chronometer Hubble data allows model-independent tests of dark energy evolution in scalar-tensor theories.
Interacting k-essence dark energy and non-pressureless dark matter models with two interaction forms are shown to reproduce major cosmological epochs and fit observations comparably to LambdaCDM while admitting late-time de Sitter attractors.
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$\text{AdS}_D\times I$ solutions in axio-dilaton gravity
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Bounding axion dark energy
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Resolving the Planck-DESI tension by nonminimally coupled quintessence
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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Exponential Quintessence: Analytic Relationship Between the Current Equation of State Parameter and the Potential Parameter
For an exponential quintessence potential, an analytic formula links the current equation-of-state w_φ0 to the potential slope λ while enforcing prior radiation and matter domination, yielding the bound λ < 1.94 at Ω_φ0 = 0.685.
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Cosmological Constraints on Minimal Cubic Galileon Models in Teleparallel Gravity
Observational constraints on teleparallel cubic Galileon cosmologies with quadratic and exponential potentials show viability for late-time acceleration, with the fixed b1 quadratic case competitive under AIC but not BIC.
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Curvature-Assisted Dynamical Compactification in a Pre-Inflationary Higher-Dimensional Universe
In a 5D open FRW model, negative curvature sustains tracker-like radion evolution that enables dynamical compactification via Casimir stabilization before 4D inflation dilutes curvature remnants.
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EFT of Dark Energy with Cosmic Chronometers: Reconstructing Background EFT Functions
Reconstruction of EFT background functions from cosmic chronometer Hubble data allows model-independent tests of dark energy evolution in scalar-tensor theories.
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Interacting $k$-essence field with non-pressureless Dark Matter: Cosmological Dynamics and Observational Constraints
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