Cosmological gravitational particle production of stable spin-3/2 raritrons yields the observed dark matter abundance across wide ranges of mass relative to the Hubble scale at the end of inflation.
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Derives the power spectrum evolution and cross-spectra for arbitrary multi-species wave and particle dark matter, incorporating free-streaming, Jeans scales, and intrinsic fluctuations.
Scalar metric perturbations after inflation break conformal invariance and induce quantum production of gravitons, generating a GW spectrum that peaks near GHz frequencies for standard primordial scalar power spectra.
Stochastic gravitational waves induce 1-loop freeze-in production of fermionic dark matter via in-in formalism, potentially explaining the observed abundance more efficiently than conventional mechanisms.
Planck CMB data set upper limits on vector and axial-vector dark matter-electron couplings for masses 100 eV to 100 keV via energy injection from inelastic scattering and hydrogen absorption.
An improved Bogoliubov numerical method computes the full primordial GW spectrum from inflation to reheating and shows that inflaton anharmonicity imprints distinctive features at high frequencies.
Canonical quantization of Proca field in Schwarzschild background with Dirac brackets, Hawking spectrum from Unruh vacuum, and numerical evaluation of condensate in three vacua.
Inflationary magnetic fields induce curvature perturbations that form ultralight PBHs, generating a stochastic GW background with model-specific features.
Certain inflation models produce right-handed neutrinos via gravitational effects sufficient for leptogenesis to explain the baryon asymmetry, testable by inflationary gravitational waves.
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.
Gravitational scalar production yields reheating-dependent constraints on dark matter scalars, with dilution preserving viability for k<4 low-temperature reheating and factorization in multi-stage cases.
PUEO will constrain the proton fraction of ultrahigh-energy cosmic rays under strong source evolution and set leading neutrino constraints on ultraheavy dark matter decays and some cosmic string models above 10^19 eV.
Updated exclusion contours on lifetime, mass and abundance of decaying BSM relics from refined BBN modeling of hadronic and electromagnetic injections across multiple two-body channels.
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.
Gravity-mediated production of scalar and vector dark radiation yields Planck 2018 constraints on reheating temperature T_RH and background equation of state w_Φ, with comparisons to right-handed neutrinos, ALPs, and a generic spin-2 mediator.
Uniformly rotating particles decay via emission of negative-energy quanta due to the lack of a global vacuum for such observers, implying none can be regarded as stable.
Gravitational vacuum polarization explains the Hubble tension by increasing direct H0 measurements while leaving indirect ones unaffected, does not impact the sigma8 tension, and predicts FRB measurements match CMB/BAO values.
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CMB Limits on the Absorption of Light Vector and Axial-Vector Dark Matter
Planck CMB data set upper limits on vector and axial-vector dark matter-electron couplings for masses 100 eV to 100 keV via energy injection from inelastic scattering and hydrogen absorption.