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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.
Forward citations
Cited by 6 Pith papers
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Perturbative Dissipation in Minimal Warm Inflation
In minimal warm inflation, perturbative dissipation from Landau damping and plasmon decay produces a third-time-derivative friction term linear in alpha, but slow-roll suppression makes it at least 10^-6 smaller than ...
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DSWIM:Efficient and Stable Deterministic Computation of Warm Inflation Perturbations
DSWIM adds a scaled deterministic correlation-matrix solver to SWIM that improves numerical conditioning for warm-inflation perturbations while exactly preserving the curvature power spectrum and resolving stochastic-...
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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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Behaviour of $\alpha$-attractors in Warm Inflation
In strongly dissipative warm inflation, T, E, and polynomial alpha-attractor models lose the cold-inflation attractor convergence in the n_s-r plane.
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Stage IV CMB forecasts for warm inflation
Future CMB surveys are forecast to tighten the dissipation parameter of quartic warm inflation by up to an order of magnitude and to exclude the cubic dissipation model under a null tensor-to-scalar ratio.
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Dark Matter Freeze-In during Warm Inflation and the Seesaw Mechanism
A U(1)_{B-L} inverse-seesaw model realizes warm-inflation freeze-in of fermionic dark matter via a heavy Z' portal, with parameters adjusted to match the observed dark matter abundance and neutrino masses.
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