Standard non-thermal leptogenesis works at arbitrarily low reheating temperatures above the BBN bound when the inflaton potential has a quartic minimum (k≥4), because the inflaton's evolving mass kinematically shuts off RHN production early.
First CMB Constraints on the Inflationary Reheating Temperature
9 Pith papers cite this work. Polarity classification is still indexing.
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abstract
We present the first Bayesian constraints on the single field inflationary reheating era obtained from Cosmic Microwave Background (CMB) data. After demonstrating that this epoch can be fully characterized by the so-called reheating parameter, we show that it is constrained by the seven years Wilkinson Microwave Anisotropies Probe (WMAP7) data for all large and small field models. An interesting feature of our approach is that it yields lower bounds on the reheating temperature which can be combined with the upper bounds associated with gravitinos production. For large field models, we find the energy scale of reheating to be higher than those probed at the Large Hadron Collider, Ereh > 17.3 TeV at 95% of confidence. For small field models, we obtain the two-sigma lower limits Ereh > 890 TeV for a mean equation of state during reheating <wreh> = -0.3 and Ereh > 390 GeV for <wreh> = -0.2. The physical origin of these constraints is pedagogically explained by means of the slow-roll approximation. Finally, when marginalizing over all possible reheating history, the WMAP7 data push massive inflation under pressure (p < 2.2 at 95% of confidence where p is the power index of the large field potentials) while they slightly favor super-Planckian field expectation values in the small field models.
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Dilaton backreaction on an anomaly-inspired axion potential generates a closed-form Lambert-W flattened hilltop, giving r ≈ 0.033–0.036 and α_s ≈ −4.6×10^{-4} at N=56 with strictly adiabatic dynamics.
Radiative corrections pull an isolated, long-lived massive graviton out of the gapped linear-dilaton continuum, giving a sub-MeV dark-matter candidate that can coexist with a holographic fluid component.
Negative field-space curvature enhances post-inflationary Ricci scalar oscillations and boosts CGPP dark matter number density by up to an order of magnitude relative to flat field-space cases, with nontrivial relic abundance dependence on spectator mass and reheating temperature.
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.
Generalized no-scale models with R=2/(3α) for α≠1 or non-minimal gauge couplings allow unsuppressed inflaton decays, producing calculable reheating temperatures and (n_s,r) predictions.
Expanded Simons Observatory could measure reheating temperature and inflaton-gluon coupling to a few percent in QCD-driven warm inflation if r=0.01 primordial gravitational waves are found.
Reheating temperature and equation-of-state parameter assumptions in Weyl-invariant Einstein-Cartan gravity models significantly alter predicted inflationary observables.
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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Leptogenesis and Low Reheating Temperatures
Standard non-thermal leptogenesis works at arbitrarily low reheating temperatures above the BBN bound when the inflaton potential has a quartic minimum (k≥4), because the inflaton's evolving mass kinematically shuts off RHN production early.
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Dilaton-Flattened Axion Inflation
Dilaton backreaction on an anomaly-inspired axion potential generates a closed-form Lambert-W flattened hilltop, giving r ≈ 0.033–0.036 and α_s ≈ −4.6×10^{-4} at N=56 with strictly adiabatic dynamics.
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Massive Graviton Dark Matter from a Gapped Continuum
Radiative corrections pull an isolated, long-lived massive graviton out of the gapped linear-dilaton continuum, giving a sub-MeV dark-matter candidate that can coexist with a holographic fluid component.
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Cosmological gravitational particle production in multifield inflation
Negative field-space curvature enhances post-inflationary Ricci scalar oscillations and boosts CGPP dark matter number density by up to an order of magnitude relative to flat field-space cases, with nontrivial relic abundance dependence on spectator mass and reheating temperature.
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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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Reheating in No-Scale Models of Inflation
Generalized no-scale models with R=2/(3α) for α≠1 or non-minimal gauge couplings allow unsuppressed inflaton decays, producing calculable reheating temperatures and (n_s,r) predictions.
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Observing Cosmic Reheating with the expanded Simons Observatory
Expanded Simons Observatory could measure reheating temperature and inflaton-gluon coupling to a few percent in QCD-driven warm inflation if r=0.01 primordial gravitational waves are found.
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Reheating in geometric Weyl-invariant Einstein-Cartan gravity
Reheating temperature and equation-of-state parameter assumptions in Weyl-invariant Einstein-Cartan gravity models significantly alter predicted inflationary observables.
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Thermal effects on Dark Matter production during cosmic reheating
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.