Clarifying inflation models: The precise inflationary potential from effective field theory and the WMAP data

Journal Article · Sun May 15 04:00:00 EDT 2005 · Physical Review. D, Particles Fields

DOI:https://doi.org/10.1103/PhysRevD.71.103518· OSTI ID:20709259

Cirigliano, D; Sanchez, N G ^[1]; Vega, H.J. de ^[1]

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1. Observatoire de Paris, LERMA, Laboratoire Associe au CNRS UMR 8112, 61, Avenue de l'Observatoire, 75014 Paris (France)

We clarify inflaton models by considering them as effective field theories in the Ginzburg-Landau spirit. In this new approach, the precise form of the inflationary potential is constructed from the present WMAP data, and a useful scheme is prepared to confront with the forthcoming data. In this approach, the WMAP statement excluding the pure {phi}{sup 4} potential implies the presence of an inflaton mass term at the scale m{approx}10{sup 13} GeV. Chaotic, new and hybrid inflation models are studied in an unified way. In all cases the inflaton potential takes the form V({phi})=m{sup 2}M{sub Pl}{sup 2}v({phi}/M{sub Pl}), where all coefficients in the polynomial v({phi}) are of order one. If such potential corresponds to supersymmetry breaking, the corresponding susy breaking scale is {radical}(mM{sub Pl}){approx}10{sup 16} GeV which turns to coincide with the grand unification (GUT) scale. The inflaton mass is therefore given by a seesaw formula m{approx}M{sub GUT}{sup 2}/M{sub Pl}. The observables turn to be two-valued functions: one branch corresponds to new inflation and the other to chaotic inflation, the branch point being the pure quadratic potential. For red tilted spectrum, the potential which fits the best the present data (vertical bar 1-n{sub s} vertical bar < or approx. 0.1,r < or approx. 0.1) and which best prepares the way for the forthcoming data is a trinomial polynomial with negative quadratic term (new inflation). For blue tilted spectrum, hybrid inflation turns to be the best choice. In both cases we find an analytic formula relating the inflaton mass with the ratio r of tensor to scalar perturbations and the spectral index n{sub s} of scalar perturbations: 10{sup 6}(m/M{sub Pl})=127{radical}(r vertical bar 1-n{sub s} vertical bar) where the numerical coefficient is fixed by the WMAP amplitude of adiabatic perturbations. Implications for string theory are discussed.

• OSTI ID: 20709259
• Journal Information: Physical Review. D, Particles Fields, Journal Name: Physical Review. D, Particles Fields Journal Issue: 10 Vol. 71; ISSN PRVDAQ; ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
AMPLITUDES
CHAOS THEORY
COSMIC RADIATION
COSMOLOGY
DISTURBANCES
GEV RANGE
GINZBURG-LANDAU THEORY
GRAND UNIFIED THEORY
INFLATIONARY UNIVERSE
PHI4-FIELD THEORY
POLYNOMIALS
POTENTIALS
RADIOWAVE RADIATION
SCALARS
STRING MODELS
SUPERSYMMETRY
SYMMETRY BREAKING
TENSORS