Warm Inflation
arXiv:astro-ph/9509049 · doi:10.1103/PhysRevLett.75.3218
Abstract
Assuming a first order phase transition during inflation, a model scenario is described which does not require a tiny coupling constant. Thermal equilibrium is closely maintained as inflation commences. No large scale reheating is necessary. Solutions for are found for any in the range .
11 pages, 2 figures (In press Physical Review Letters 1995)
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- Fresh inflation from five-dimensional vacuum state
- Revisiting Barrow's Graduated Inflationary Universe: A Warm perspective
- Phantom cosmology with arbitrary potential: New accelerating scaling attractors
- Discrepancies between observational data and theoretical forecast in single field slow roll inflation
- Scalaron-driven Dark Matter during Warm Inflation via UV Freeze--in
- Evolution of superhorizon perturbations in early Universe with anisotropic solid remnant
- Condensate decay in a radiation dominated cosmology
- Warm inflation: Towards a realistic COBE data power spectrum for matter and metric thermal coupled fluctuations
- The spectrum of tensor perturbations in warm inflation
- Theoretical and observational aspects of cosmological inflation
- AliCPT Sensitivity to Cosmic Reheating
- Inflation and primordial fluctuations in gravity
- Not So Minimal Warm Inflation
- Thermal enhancement of inflationary magnetic fields
- Warming up D3 brane motion in the background of D5 brane and Inflation
- Complex Inflaton Potentials with Nonminimal Coupling: Robust Inflation and Geometric Reheating
- Dynamics of potential-free warm -inflation with nonminimal derivative coupling