Radiative corrections from spectator fields cause the inflaton to evolve as an exponential of N_e squared during slow-roll inflation, unlike linear friction approximations, while producing spectator particles whose total number grows exponentially with e-folds.
The Origin of Matter in the Universe: Reheating after Inflation
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In the inflationary scenario all the matter constituting the universe was created from the process of reheating after inflation. Recent development of the theory of reheating is briefly reviewed. The list of topics includes elementary (perturbative) theory of reheating; quantum field theory in a time-varying background; parametric resonance and explosive particle creation; non-thermal phase transitions from reheating; baryogenesis from reheating; residual oscillations of the scalar field, and other cosmological applications.
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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.
Lecture notes providing a generic introduction to reheating after inflation, covering its theoretical, phenomenological, and observational aspects.
citing papers explorer
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What spectators do during inflation
Radiative corrections from spectator fields cause the inflaton to evolve as an exponential of N_e squared during slow-roll inflation, unlike linear friction approximations, while producing spectator particles whose total number grows exponentially with e-folds.
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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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Lectures on Reheating after Inflation
Lecture notes providing a generic introduction to reheating after inflation, covering its theoretical, phenomenological, and observational aspects.