Dissipation of small-scale primordial perturbations after neutrino decoupling cools relic neutrinos and reduces their abundance, enabling PTOLEMY to constrain the primordial curvature power spectrum to O(0.1) on scales k ≲ 3×10^5 Mpc^{-1}.
Recent Advances in Inflation
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Higher-curvature gravities are constructed in which both FLRW backgrounds and linearized scalar perturbations obey at most second-order differential equations.
Non-Gaussian primordial fluctuations of a Z2-symmetric spectator scalar trigger a strong first-order electroweak phase transition, with the field serving as cold dark matter and generating a stochastic gravitational wave background in the 10^{-3}-10^{-1} Hz band.
Authors add induced gravity and a polynomial potential to an F(R) model, transform to a two-field chiral cosmology, and find parameter choices that match ACT inflation data while yielding PBH masses compatible with dark matter.
Exponential and sech Gauss–Bonnet couplings restore ACT-compatible ns and r for quintessential inflation, while tanh fails for a structural sign reason; reheating remains BBN-safe.
In f(Q,φ) gravity with nonminimal coupling, De Sitter inflation works only for 10^{-3} ≲ ξ ≲ 10^{-2} while a Cosh model gives ns ≈ 0.965-0.967 and r ≈ 0.017-0.018 at N=60, matching observations.
Bouncing solutions in quadratic curvature gravity with a scalar field satisfy null, weak, and dominant energy conditions but violate the strong one when using the scalar-field energy-momentum tensor, while all four conditions are violated near the bounce in the effective tensor formulation.
Ghost-free non-local gravity fits Pantheon+, DESI, and H(z) data but fails with added CMB, while generalized exponential F(R) gravity outperforms Lambda CDM across all datasets including CMB.
citing papers explorer
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Probing the small-scale primordial power spectrum via relic neutrinos and acoustic reheating
Dissipation of small-scale primordial perturbations after neutrino decoupling cools relic neutrinos and reduces their abundance, enabling PTOLEMY to constrain the primordial curvature power spectrum to O(0.1) on scales k ≲ 3×10^5 Mpc^{-1}.
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Cosmological higher-curvature gravities
Higher-curvature gravities are constructed in which both FLRW backgrounds and linearized scalar perturbations obey at most second-order differential equations.
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Electroweak First-Order Phase Transition Triggered by Non-Gaussian Fluctuations of a $\mathbb{Z}_2$-Symmetric Spectator Scalar
Non-Gaussian primordial fluctuations of a Z2-symmetric spectator scalar trigger a strong first-order electroweak phase transition, with the field serving as cold dark matter and generating a stochastic gravitational wave background in the 10^{-3}-10^{-1} Hz band.
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Primordial black holes formation in inflationary $F(R)$ models with scalar fields
Authors add induced gravity and a polynomial potential to an F(R) model, transform to a two-field chiral cosmology, and find parameter choices that match ACT inflation data while yielding PBH masses compatible with dark matter.
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Constraining Quintessential Inflation with ACT: A Gauss-Bonnet Gateway
Exponential and sech Gauss–Bonnet couplings restore ACT-compatible ns and r for quintessential inflation, while tanh fails for a structural sign reason; reheating remains BBN-safe.
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Inflationary Scenarios in $f(Q,\phi)$ Gravity with Scalar Field Coupling
In f(Q,φ) gravity with nonminimal coupling, De Sitter inflation works only for 10^{-3} ≲ ξ ≲ 10^{-2} while a Cosh model gives ns ≈ 0.965-0.967 and r ≈ 0.017-0.018 at N=60, matching observations.
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Energy conditions of bouncing solutions in quadratic curvature gravity coupled with a scalar field
Bouncing solutions in quadratic curvature gravity with a scalar field satisfy null, weak, and dominant energy conditions but violate the strong one when using the scalar-field energy-momentum tensor, while all four conditions are violated near the bounce in the effective tensor formulation.
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Dark Energy in Ghost-free non-local Gravity
Ghost-free non-local gravity fits Pantheon+, DESI, and H(z) data but fails with added CMB, while generalized exponential F(R) gravity outperforms Lambda CDM across all datasets including CMB.