Reheating and Preheating after Inflation
| dc.creator | Kofman, Lev | |
| dc.date | 1998-02-10 | |
| dc.date.accessioned | 2026-07-07T04:03:27Z | |
| dc.date.available | 2026-07-07T04:03:27Z | |
| dc.description | It is assumed that during inflation, all energy was contained in a slow-rolling inflaton field $ϕ$. The particles constituting the Universe are created due to interactions with the field $ϕ$ coherently oscillating after inflation. The leading channel of the particle production would be the non-perturbative regime of parametric resonance, preheating. Some of the recent developments in the theory of preheating are briefly reviewed. As a prototype we use the model ${λ\over 4}ϕ^4 + {m^2 \over 2}ϕ^2+ {g^2\over 2}ϕ^2χ^2$ in an expanding universe. In different domains of parameters the character of preheating $(ϕ\to χ)$ or $(ϕ\to δϕ)$ is different, ranging from regular Lamé to stochastic parametric resonances. Fortunately, in many important cases simple analytic resonant solutions are found. Eventually, a picture which unifies the different regimes emerges. | |
| dc.description | 8 pages, in: 3rd RESCEU Symp. Particle Cosmology, Tokyo 1997 | |
| dc.identifier | https://arxiv.org/abs/hep-ph/9802285 | |
| dc.identifier | http://arxiv.org/abs/hep-ph/9802285 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/47662 | |
| dc.subject | High Energy Physics - Phenomenology | |
| dc.subject | Astrophysics | |
| dc.subject | High Energy Physics - Theory | |
| dc.title | Reheating and Preheating after Inflation | |
| dc.type | text |