Cosmological inflation is frequently associated with a scalar field φ, which could also generate GN, via a coupling term 1/2 ɛ φ2 R in the lagrangian, as a result of symmetry breaking. We derive a formula for density perturbations δϱ//ϱ in the theory L = [(16πG0)-1 + 1/2ɛφ2]R + 1/2ɛkφk -V(φ). When G0-1 = 0, our results largely coincide with those of Accetta, Zoller and Turner, who assumed a Ginzburg-Landau potential V = 1/4λ(φ2 - φ02)2 and the formula δϱ//ϱ = αH2//φ. We verify that formula and find the constant of proportionality to be α ~ 2 × 10-2.
Inflation with a Non--Minimally Coupled Scalar Field
LUCCHIN, FRANCESCO;MATARRESE, SABINO;
1986
Abstract
Cosmological inflation is frequently associated with a scalar field φ, which could also generate GN, via a coupling term 1/2 ɛ φ2 R in the lagrangian, as a result of symmetry breaking. We derive a formula for density perturbations δϱ//ϱ in the theory L = [(16πG0)-1 + 1/2ɛφ2]R + 1/2ɛkφk -V(φ). When G0-1 = 0, our results largely coincide with those of Accetta, Zoller and Turner, who assumed a Ginzburg-Landau potential V = 1/4λ(φ2 - φ02)2 and the formula δϱ//ϱ = αH2//φ. We verify that formula and find the constant of proportionality to be α ~ 2 × 10-2.File in questo prodotto:
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