Asymmetric reheating in Dark QED produces dark matter via a new channel where DM particles annihilate while still being created by inflaton decay, with the hidden-to-visible temperature ratio tied to the square root of the Yukawa coupling ratio.
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6 Pith papers cite this work. Polarity classification is still indexing.
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Simulations in Einstein-scalar-Gauss-Bonnet gravity show oscillons form with similar properties to standard cases but trigger EFT breakdown for large couplings via high local curvatures.
Stronger couplings or inflaton-seeded initial abundance allow freeze-in dark matter to match the relic density while evading DAMIC-M and PandaX bounds for reheating temperatures below the electroweak scale.
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.
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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Asymmetric Reheating of Dark QED
Asymmetric reheating in Dark QED produces dark matter via a new channel where DM particles annihilate while still being created by inflaton decay, with the hidden-to-visible temperature ratio tied to the square root of the Yukawa coupling ratio.
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Preheating and oscillon formation in Einstein-scalar-Gauss-Bonnet gravity
Simulations in Einstein-scalar-Gauss-Bonnet gravity show oscillons form with similar properties to standard cases but trigger EFT breakdown for large couplings via high local curvatures.
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When direct detection constrains reheating temperature: freeze-in with stronger couplings and inflaton-seeded freeze-in
Stronger couplings or inflaton-seeded initial abundance allow freeze-in dark matter to match the relic density while evading DAMIC-M and PandaX bounds for reheating temperatures below the electroweak scale.
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Analytic Approximations for Fermionic Preheating
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.
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Gravitational Waves from Matter Perturbations of Spectator Scalar Fields
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.
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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.