1998/02/17 by Lev Kofman, Kofman, Lev
Physics and Astronomy · #Astrophysics (astro-ph) #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #High Energy Physics - Phenomenology (hep-ph) #High Energy Physics - Theory (hep-th) #astro-ph #hep-ph #hep-th
paper · pdf · doi:10.48550/arxiv.astro-ph/9802221
11 pages, 2 figs, based on a talk in the proceedings of the Workshop on Particle Physics and the Early Universe, Cosmo97 Ambleside, September 1997, Ed. L. Roszkowski
arxiv created 1998/02/17 · openalex publication_date 1998/02/17 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In inflationary cosmology, the particles constituting the Universe are created after inflation in the process of reheating due to the interaction with the oscillating inflaton field. We briefly review the basics of the slow reheating, and the stage of fast preheating, when the particles are created explosively in the regime of parametric resonance. The non-perturbative, out-of-equilibrium character of the parametric resonance changes many features of reheating. For these proceedings, we will highlight a few aspects of preheating: the structural dependence of the parametric resonance on the inflationary model, including V(ϕ)=m2 \over 2ϕ2, λ\over 4ϕ4, 1-cos ϕ\over f; ``rescattering'' of created particles; and phase transitions after inflation.