Derives integro-differential boundary equations from bulk locality for scale-breaking cosmological correlators with oscillating heavy-field masses and solves them analytically and numerically to reveal enhanced collider signals.
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Reheating after Inflation
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abstract
The theory of reheating of the Universe after inflation is developed. The transition from inflation to the hot Universe turns out to be strongly model-dependent and typically consists of several stages. Immediately after inflation the field $\phi$ begins rapidly rolling towards the minimum of its effective potential. Contrary to some earlier expectations, particle production during this stage does not lead to the appearance of an extra friction term $\Gamma\dot\phi$ in the equation of motion of the field $\phi$. Reheating becomes efficient only at the next stage, when the field $\phi$ rapidly oscillates near the minimum of its effective potential. We have found that typically in the beginning of this stage the classical inflaton field $\phi$ very rapidly (explosively) decays into $\phi$-particles or into other bosons due to broad parametric resonance. This stage cannot be described by the standard elementary approach to reheating based on perturbation theory. The bosons produced at this stage, as well as some part of the classical field $\phi$ which survives the stage of explosive reheating, should further decay into other particles, which eventually become thermalized. The last stages of decay can be described in terms of perturbation theory. Complete reheating is possible only in those theories where a single massive $\phi$-particle can decay into other particles. This imposes strong constraints on the structure of inflationary models. On the other hand, this means that a scalar field can be a cold dark matter candidate even if it is strongly coupled to other fields.
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representative citing papers
An oscillating homogeneous SU(2) condensate indirectly induces parametric resonance in U(1) helicity modes via a pseudoscalar mediator, producing a Hill equation that reduces to Mathieu form with derived resonance conditions and a non-chiral property in the periodic limit.
Mixing of ultralight wave dark matter fields creates a wave-envelope structure with intrinsic slow modulation and frequency sidebands, violating the standard monochromatic assumption.
Curvaton self-interactions in non-quadratic potentials produce a local non-Gaussian map that enables supermassive primordial black hole formation at peak amplitudes of order 10^{-5} while remaining consistent with μ-distortion bounds.
Resonant exponential growth of millicharged scalars in k²>0 electromagnetic waves is obtained by mapping the Klein-Gordon equation to the Mathieu equation, yielding new constraints on such particles.
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.
Constructs an explicit closed FRW curvature-supported bounce-inflation model with a canonical scalar field that remains geodesically complete, NEC-compliant, and yields standard slow-roll predictions.
Lattice QCD computations in thermal effective field theory yield sphaleron rates and axion production rates that deviate from perturbative estimates at high temperatures.
Post-inflationary axion-SU(2) vector dark matter production is recast as a quantum quench with a survival factor that induces an O(1) renormalization of the standard relic abundance.
Axion-like particles in the trapped misalignment mechanism produce observable gravitational waves while generating intergalactic magnetic fields that exceed blazar lower bounds in the parameter space promising for gravitational wave detection.
Inflaton accretion during reheating drives non-linear PBH mass growth that extends lifetimes and amplifies emitted SGWB by multiple orders of magnitude.
Perturbative inflaton decay emits an irreducible stochastic GW background with Ω_GW ∝ f spectrum whose amplitude is set by the hard decay rate and reaches O(10^{-17}) at GHz scales.
Deformed alpha-attractor T-models with a Gaussian feature near the minimum yield more smaller shorter-lived oscillons during self-resonance preheating, suppressing energy in oscillons and altering the high-frequency gravitational wave tail while leaving low frequencies unchanged.
High-frequency primordial gravitational waves extend to higher frequencies due to post-inflation inflaton dynamics, and their detailed spectrum shape can distinguish inflation models.
Thermal bath corrections derived via thermofield dynamics enhance the evaporation rate of primordial black holes, shortening their lifetimes relative to zero-temperature calculations.
Dark matter freezes in from non-thermal Z' decays before reheating ends in an inflationary model with a secluded U(1)_D gauge sector, Z' reheaton, and lattice treatment of non-perturbative effects, opening viable parameter space with GW probes.
Lattice simulations show that the post-inflationary equation of state with trilinear interactions returns to zero after an initial deviation, substantially lowering stochastic gravitational wave amplitudes relative to prior estimates.
K-inflation with non-canonical kinetic term G(φ) shifts α-attractor T-models and natural inflation into the Planck-ACT-LB-BK18 allowed region while satisfying Swampland conjectures and producing testable GW spectra.
Torsion-induced fermion condensate produces hybrid inflation with axial-chemical-potential waterfall, Q-ball PBH seeds, and parity-violating signatures in Chern-Simons gravity.
Analytic approximations for fermion number density in λφ⁴ preheating scale as q^{1/2} for q ≲ 0.01 and q^{3/4} for q ≳ 10, with resonance peaks or half-filled Fermi spheres depending on the coupling.
A spectator scalar field with strong portal coupling to the inflaton sources a stochastic gravitational wave background reaching Ω_GW h² ∼ 10^{-11} at frequencies 10^7-10^8 Hz for benchmark parameters σ/λ ≃ 10^4 and T_reh = 2×10^{14} GeV.
Two minimal single-parameter extensions of the α-Starobinsky model shift ns into the 1σ ACT DR6 region while keeping r < 0.038 and yielding T_re ~ 10^9 GeV for N_k in [50,65].
Differences in inflationary energy scales between Einstein and Jordan frames produce distinct reheating e-folding numbers and temperatures, leading to contrasting thermal histories with potential observational signatures.
Thermal corrections to reheating and freeze-in DM production rates are generally small in the computable regime but can be large in constructed counter-examples.
citing papers explorer
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Memoirs of the curvaton: non-perturbative non-Gaussianity and supermassive primordial black holes
Curvaton self-interactions in non-quadratic potentials produce a local non-Gaussian map that enables supermassive primordial black hole formation at peak amplitudes of order 10^{-5} while remaining consistent with μ-distortion bounds.
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Precision Inflationary Predictions: Impact of Accurate End-of-Inflation Dynamics
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.
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Geodesically Complete Curvature-Bounce Inflation
Constructs an explicit closed FRW curvature-supported bounce-inflation model with a canonical scalar field that remains geodesically complete, NEC-compliant, and yields standard slow-roll predictions.
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Inflaton Accretion onto Primordial Black Holes During Reheating
Inflaton accretion during reheating drives non-linear PBH mass growth that extends lifetimes and amplifies emitted SGWB by multiple orders of magnitude.
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Self-resonance preheating in deformed attractor models: oscillon formation and evolution
Deformed alpha-attractor T-models with a Gaussian feature near the minimum yield more smaller shorter-lived oscillons during self-resonance preheating, suppressing energy in oscillons and altering the high-frequency gravitational wave tail while leaving low frequencies unchanged.
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Equation of state during (p)reheating with trilinear interactions
Lattice simulations show that the post-inflationary equation of state with trilinear interactions returns to zero after an initial deviation, substantially lowering stochastic gravitational wave amplitudes relative to prior estimates.
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Minimal Extensions of the $\alpha$-Starobinsky Model: Reconciling ACT DR6 and Reheating Constraints
Two minimal single-parameter extensions of the α-Starobinsky model shift ns into the 1σ ACT DR6 region while keeping r < 0.038 and yielding T_re ~ 10^9 GeV for N_k in [50,65].
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ACT DR6+Planck impact on inflation with non-zero vacuum expectation value and the post-inflationary behavior
Updated constraints on non-zero VEV parameter M from ACT+Planck data, plus lattice simulations showing oscillon formation and reheating implications.
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Science Case for the Einstein Telescope
The Einstein Telescope will enable gravitational-wave observations up to cosmological distances, opening avenues for discoveries in astrophysics, cosmology, and fundamental physics.
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Lectures on Reheating after Inflation
Lecture notes providing a generic introduction to reheating after inflation, covering its theoretical, phenomenological, and observational aspects.
- Constraining Quintessential Inflation with ACT: A Gauss-Bonnet Gateway