Dependence of cosmological energy-density irregularities on the shape of the scalar-field potential during inflation and reheating''

Journal Article · Mon Jul 15 00:00:00 EDT 1991 · Physical Review, D (Particles Fields); (USA)

DOI:https://doi.org/10.1103/PhysRevD.44.365· OSTI ID:5666458

Ratra, B ^[1]

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1. Theoretical Astrophysics and Theoretical Physics, California Institute of Technology, Pasadena, California 91125 (USA)

Estimates for the baryon-dominated epoch form of the large-scale adiabatic energy-density irregularities generated during an early scalar-field-dominated inflation epoch, in simple inflation-modified hot-big-bang models, are compared to the widely used approximate general expression, which is proportional to the large-scale, gauge-invariant part of {ital H}{sup 2}{l angle}{phi}{phi}{sup *}{r angle}/({dot {Phi}}{sub {ital b}}){sup 2} evaluated at the first Hubble radius crossing (here {Phi}{sub {ital b}} and {phi} are the spatially homogeneous and inhomogeneous parts of the scalar field, {ital H} is the Hubble parameter, and an overdot represents a derivative with respect to time). In the de Sitter inflation limit, if the inflation-epoch background scalar-field solution is an attractor,'' or if there is sufficient inflation before the scale of interest leaves the Hubble radius, the approximate general expression identically reproduces what we have found. It is also less than an order of magnitude away from our expression in a large fraction of the parameter space of the inflation model we study and is within 2 orders of magnitude of our result in almost all of parameter space. We also show that the more accurate general expression (which the above formula is an approximation of) identically reproduces our results in the simple models studied, provided the inflation-epoch background scalar-field solution is an attractor'' or if there is sufficient inflation. The approximate general formula is used to restudy energy-density inhomogeneities in the quartic-potential scalar-field de Sitter inflation model; the difference between the standard result in this model and our result in related models is traced to a difference in the form of the part of the potential used to model reheating'' and the end of inflation.

• DOE Contract Number: AC03-81ER40050
• OSTI ID: 5666458
• Journal Information: Physical Review, D (Particles Fields); (USA), Vol. 44:2; ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
COSMOLOGICAL MODELS
SCALAR FIELDS
ENERGY DENSITY
EQUATIONS OF MOTION
GAUGE INVARIANCE
HUBBLE EFFECT
INFLATIONARY UNIVERSE
RED SHIFT
RENORMALIZATION
SPACE-TIME
UNIVERSE
DIFFERENTIAL EQUATIONS
EQUATIONS
INVARIANCE PRINCIPLES
MATHEMATICAL MODELS
PARTIAL DIFFERENTIAL EQUATIONS
640106* - Astrophysics & Cosmology- Cosmology
645400 - High Energy Physics- Field Theory
645300 - High Energy Physics- Particle Invariance Principles & Symmetries