Chaotic reheating
| dc.creator | Podolsky, D. I. | |
| dc.creator | Starobinsky, A. A. | |
| dc.date | 2002-04-19 | |
| dc.date.accessioned | 2026-07-07T02:03:28Z | |
| dc.date.available | 2026-07-07T02:03:28Z | |
| dc.description | We discuss the structure of parametric resonance which occurs in the process of reheating after inflation with two interacting scalar fields. It is found that, for the case of a not too large coupling constant, a quasi-homogeneous part of the second, initially subdominant scalar field may not be neglected due to its stochastic growth during inflation. This fact has strong consequences for the reheating stage: dynamics of background fields becomes chaotic after inflation -- it consists of subsequent chaotic and regular eras, and a tachyonic instability for inhomogeneous perturbations arises in the quantum reheating problem. This instability may pose a problem for the standard reheating scenario. In order to avoid it, the coupling constant should be either sufficiently small, or very large. | |
| dc.description | Talk at the COSMION-5 conference (Moscow, 21-30 May 2001). To be published in Gravit. & Cosmology, 2002, Vol. 8, Suppl. 6 pages, latex with the cosmion.sty | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0204327 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0204327 | |
| dc.identifier | Grav.Cosmol.Suppl. 8N1 (2002) 13-18 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/4391 | |
| dc.subject | Astrophysics | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.subject | High Energy Physics - Phenomenology | |
| dc.title | Chaotic reheating | |
| dc.type | text |