Inflation with a non-minimally coupled scalar field

Details Inflation with a non-minimally coupled scalar field Inflation with a non-minimally coupled scalar field

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986phlb..167..163l&link_type=abstract

Physics Letters B, Volume 167, Issue 2, p. 163-168.

Physics

46

Scientific paper

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.

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