Initial condition of scalar perturbation in inflation

Abstract

A formula for the power spectrum of curvature perturbations having any initial conditions in inflation is obtained. Based on the physical conditions before inflation, the possibility exists that the initial state of scalar perturbations is not only the Bunch-Davies state, but also a more general state (a squeezed state). For example, the derived formula for the power spectrum is calculated using simple toy cosmological models. When there exists a radiation-dominated period before inflation, the behavior of the scalar perturbation is revealed not to vary greatly; however, from large scales to small scales the power spectrum of the curvature perturbations oscillates around the normal value. In addition, when inflation has a large break and the breaking time is a radiation- dominated period, a large enhancement is revealed to occur which depends on the length of the breaking time.

24 pages,3 figues

References in corpus (3)

• Enhancement of superhorizon scale inflationary curvature perturbations
• The Density Perturbation Power Spectrum to Second-Order Corrections in the Slow-Roll Expansion
• Short Distance Physics and the Consistency Relation for Scalar and Tensor Fluctuations in the Inflationary Universe

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• Thermal gravitational-wave background in the general pre-inflationary scenario
• Lowering tensor-to-scalar ratio by pre-inflationary dynamics