Shape of the inflaton potential and the efficiency of the universe heating
arXiv:1412.0112 · doi:10.1140/epjc/s10052-015-3666-4
Abstract
It is shown that the efficiency of the universe heating by an inflaton field depends not only on the possible presence of parametric resonance in the production of scalar particles but also strongly depends on the character of the inflaton approach to its mechanical equilibrium point. In particular, when the inflaton oscillations deviate from pure harmonic ones toward a succession of step functions, the production probability rises by several orders of magnitude. This in turn leads to a much higher temperature of the universe after the inflaton decay, in comparison to the harmonic case. An example of the inflaton potential is presented which creates a proper modification of the evolution of the inflaton toward equilibrium and does not destroy the nice features of inflation.
14 pages, 12 figures; final version published in EPJC
References in corpus (10)
- Monodromy in the CMB: Gravity Waves and String Inflation
- Reheating in Inflationary Cosmology: Theory and Applications
- Nonperturbative Dynamics Of Reheating After Inflation: A Review
- New models of chaotic inflation in supergravity
- Axions as Quintessence in String Theory
- End of inflation, oscillons and matter-antimatter asymmetry
- Preheating after N-flation
- A Theory of Self-Resonance After Inflation, Part 1: Adiabatic and Isocurvature Goldstone Modes
- On the Suppression of Parametric Resonance and the Viability of Tachyonic Preheating after Multi-Field Inflation
- A Theory of Self-Resonance After Inflation, Part 2: Quantum Mechanics and Particle-Antiparticle Asymmetry