Published July 21, 2002 | Version v1
Journal article

Effect of inflation on parametric resonance during preheating

Creators

  • 1. Osaka Electro-Communication Junior College, Neyagawa, Osaka 572-8530 (Japan)

Description

The effect of inflation on parametric resonance during preheating is investigated. The behaviour of the preheating scalar field during inflation is investigated and is found to become squeezed in cases ranging from small-scale cases to large-scale cases. However, the positive-frequency solution is usually adopted in the initial condition of the scalar field at preheating. Although large squeezing occurs during inflation, the difference in the comoving occupation number of particles nk between two initial conditions is shown to be not so large. Rather, the ratio nk varies from 0.2 to 5.0, depending on k. In order to clarify this situation, we introduce the squeeze formulation. The squeeze parameters r and φ are calculated not only in preheating, but also in inflation. Since the squeeze parameters are calculated from inflation to preheating, we can clarify the behaviour of the parametric resonance. In preheating, the behaviour of r is shown to remain relatively unchanged with respect to k; however, the squeeze angle φ displays different behaviour for large-scale cases and small-scale cases

Availability note (English)

Available online at http://stacks.iop.org/0264-9381/19/3665/q21408.pdf or at the Web site for the journal Classical and Quantum Gravity (ISSN 1361-6382) http://www.iop.org/

Additional details

Identifiers

Publishing Information

Journal Title
Classical and Quantum Gravity
Journal Volume
19
Journal Issue
14
Journal Page Range
p. 3665-3677
ISSN
0264-9381
CODEN
CQGRDG

INIS

Country of Publication
United Kingdom
Country of Input or Organization
International Atomic Energy Agency (IAEA)
INIS RN
34033060
Subject category
S72: PHYSICS OF ELEMENTARY PARTICLES AND FIELDS;
Descriptors DEI
FIELD THEORIES; INFLATIONARY UNIVERSE; PARAMETRIC ANALYSIS; RESONANCE; SCALAR FIELDS
Descriptors DEC
COSMOLOGICAL MODELS; MATHEMATICAL MODELS