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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Kolb and A.J
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abstract
Cosmological gravitational particle production (CGPP) is the creation of particles in an expanding universe due solely to their gravitational interaction. These particles can play an important role in the cosmic history through their connection to various cosmological relics including dark matter, gravitational wave radiation, dark radiation, and the baryon asymmetry. This review explains the phenomenon of CGPP as a consequence of quantum fields in a time-dependent background, catalogs known results for the spectra and cosmological abundance of gravitationally produced particles of various spins, and explores the phenomenological consequences and observational signatures of CGPP.
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representative citing papers
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.
Starobinsky supergravity coupled to the MSSM links the CMB inflationary scale to the Higgs boson mass (~125 GeV) and predicts thermal wino dark matter at ~3 TeV, testable at future colliders and direct detection experiments.
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.
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.
For n=2 inflaton potentials Boltzmann and Bogoliubov agree on short-wavelength gravitons; for n>2 the non-adiabatic transition dominates and requires the Bogoliubov formalism.
Derives expressions connecting particle production from metric perturbations to the stress-energy tensor correlator and establishes a phenomenological link between dark matter yield and stochastic gravitational wave background amplitude for sub-horizon sources.
Generalizes UFO to T ~ a^{-ξ} and introduces GUFO from gravitational production, extending DM mass reach to 10^7 GeV for n=2 in matter-like reheating.
The QSL framework generates a geometric Dirac mass M_eff = (1/√6)|χ̇/χ| for spin-1/2 fermions from gravitational freeze-in, locked to H_* so that relic abundance depends on essentially one scale.
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.
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.
QFT in FLRW spacetime yields a running vacuum energy density ρ_vac(H) that unifies mild dynamical dark energy today with H^4 inflation without an inflaton field.
citing papers explorer
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Creation of spin-3/2 dark matter via cosmological gravitational particle production
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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Growth of Structure in Multi-species Wave Dark Matter
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.
-
Quantum production of gravitational waves after inflation
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.
-
Gravitational Wave-Induced Freeze-In of Fermionic Dark Matter
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.
-
Higgs boson mass and thermal wino dark matter from Starobinsky supergravity with the MSSM
Starobinsky supergravity coupled to the MSSM links the CMB inflationary scale to the Higgs boson mass (~125 GeV) and predicts thermal wino dark matter at ~3 TeV, testable at future colliders and direct detection experiments.
-
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.
-
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.
-
Graviton Production from Inflaton Condensate: Boltzmann vs Bogoliubov
For n=2 inflaton potentials Boltzmann and Bogoliubov agree on short-wavelength gravitons; for n>2 the non-adiabatic transition dominates and requires the Bogoliubov formalism.
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Particle Production from Inhomogeneities: the off-shell side of gravitational waves
Derives expressions connecting particle production from metric perturbations to the stress-energy tensor correlator and establishes a phenomenological link between dark matter yield and stochastic gravitational wave background amplitude for sub-horizon sources.
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Gravitational ultra-relativistic freeze-out during general reheating
Generalizes UFO to T ~ a^{-ξ} and introduces GUFO from gravitational production, extending DM mass reach to 10^7 GeV for n=2 in matter-like reheating.
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Dark matter from the quadratic spinor Lagrangian I: Geometric mass for a gravitationally produced spin-1/2 fermion
The QSL framework generates a geometric Dirac mass M_eff = (1/√6)|χ̇/χ| for spin-1/2 fermions from gravitational freeze-in, locked to H_* so that relic abundance depends on essentially one scale.
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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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Canonical quantization of massive vector field in Schwarzschild black hole background
Canonical quantization of Proca field in Schwarzschild background with Dirac brackets, Hawking spectrum from Unruh vacuum, and numerical evaluation of condensate in three vacua.
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The Magnetic Origin of Primordial Black Holes: Ultralight PBHs and Secondary GWs
Inflationary magnetic fields induce curvature perturbations that form ultralight PBHs, generating a stochastic GW background with model-specific features.
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Nonthermal leptogenesis via cosmological gravitational particle production is tested by inflationary gravitational waves
Certain inflation models produce right-handed neutrinos via gravitational effects sufficient for leptogenesis to explain the baryon asymmetry, testable by inflationary gravitational waves.
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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.
-
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.
-
Gravitational scalar production with a generic reheating scenario
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.
-
The Sensitivity of PUEO to Cosmogenic Neutrinos and Exotic Physics Scenarios
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.
-
Improved Big Bang Nucleosynthesis constraints on decaying massive relics
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 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.
-
CMB signatures of gravity-mediated dark radiation in $\mathbf{\Delta N_{\rm eff}}$
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.
-
Decay of uniformly rotating particles
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.
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Running Vacuum in the expanding Universe: a unified QFT paradigm for Inflation and Dark Energy
QFT in FLRW spacetime yields a running vacuum energy density ρ_vac(H) that unifies mild dynamical dark energy today with H^4 inflation without an inflaton field.
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Gravitational particle production, the cosmological tensions and fast radio bursts
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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From inflation to hot big bang -- a tutorial on cosmological perturbations
A tutorial deriving cosmological perturbation equations from inflation through reheating, with explicit gauge-invariant computations and Python scripts.
- A Unified Bogoliubov Approach to Primordial Gravitational Waves: From Inflation to Reheating