In warm inflation with Υ∝T³, a residual inflaton condensate after rapid drop in Q evolves as cold dark matter with mass fixed at m≈0.02 MeV by the observed abundance.
Scalar perturbation spectra from warm inflation
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abstract
We present a numerical integration of the cosmological scalar perturbation equations in warm inflation. The initial conditions are provided by a discussion of the thermal fluctuations of an inflaton field and thermal radiation using a combination of thermal field theory and thermodynamics. The perturbation equations include the effects of a damping coefficient $\Gamma$ and a thermodynamic potential $V$. We give an analytic expression for the spectral index of scalar fluctuations in terms of a new slow-roll parameter constructed from $\Gamma$. A series of toy models, inspired by spontaneous symmetry breaking and a known form of the damping coefficient, lead to a spectrum with $n_s>1$ on large scales and $n_s<1$ on small scales.
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astro-ph.CO 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
DSWIM adds a Hubble-scaled deterministic correlation matrix evolution to SWIM that preserves the primordial curvature power spectrum exactly while improving numerical conditioning and resolving stochastic-deterministic discrepancies.
citing papers explorer
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Dark Matter as an Inflationary Relic in Warm Inflation
In warm inflation with Υ∝T³, a residual inflaton condensate after rapid drop in Q evolves as cold dark matter with mass fixed at m≈0.02 MeV by the observed abundance.
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DSWIM:Efficient and Stable Deterministic Computation of Warm Inflation Perturbations
DSWIM adds a Hubble-scaled deterministic correlation matrix evolution to SWIM that preserves the primordial curvature power spectrum exactly while improving numerical conditioning and resolving stochastic-deterministic discrepancies.