Scalar field potential in inflationary models: Reconstruction and further constraints.

Abstract

We present quantitative constraints on the scalar field potential for a general class of inflationary models. (1) We first study aspects of the reconstruction of the inflationary potential from primordial fluctuation spectra. Specifically, we consider the case of a pure power law spectrum for the total perturbations (density modes as well as tensor gravitational modes); for this case the reconstruction of the potential can be done semianalytically. We find the solutions and present a series of figures. The figures show how the shape of the potential depends on the shape of the perturbation spectrum and on the relative contribution of tensor modes and scalar density perturbations. When tensor modes provide a significant fraction of the total, the potentials V(\ensuremath{\varphi}) are concave upward; when tensor modes provide a negligible contribution, the potentials are concave downward. (2) We show that the ratio scrR of the amplitude of tensor perturbations (gravity wave perturbations) to scalar density perturbations is bounded from above: scrR\ensuremath{\le}6.1. We also show that the average ratio 〈scrR〉 is proportional to the change \ensuremath{\Delta}\ensuremath{\varphi} in the field: 〈scrR〉\ensuremath{\approxeq}1.6\ensuremath{\Delta}\ensuremath{\varphi}/${\mathit{M}}_{\mathrm{Pl}}$. Thus, if tensor perturbations are important for the formation of structure, then the width \ensuremath{\Delta}\ensuremath{\varphi} must be comparable to the Planck mass. (3) We constrain the change \ensuremath{\Delta}V of the potential and the change \ensuremath{\Delta}\ensuremath{\varphi} of the inflation field during the portion of inflation when cosmological structure is produced.