Computing the Primordial Power Spectra Directly
arXiv:1207.3227 · doi:10.1088/1475-7516/2012/08/029
Abstract
The tree order power spectra of primordial inflation depend upon the norm-squared of mode functions which oscillate for early times and then freeze in to constant values. We derive simple differential equations for the power spectra, that avoid the need to numerically simulate the physically irrelevant phases of the mode functions. We also derive asymptotic expansions which should be valid until a few e-foldings before first horizon crossing, thereby avoiding the need to evolve mode functions from the ultraviolet over long periods of inflation.
11 pages, uses LaTex2e
References in corpus (5)
- Bayesian Analysis of Inflation II: Model Selection and Constraints on Reheating
- Bayesian Analysis of Inflation: Parameter Estimation for Single Field Models
- The Zeta-Zeta Correlator Is Time Dependent
- Issues Concerning Loop Corrections to the Primordial Power Spectra
- Possible Enhancement of High Frequency Gravitational Waves
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- Precision Predictions for the Primordial Power Spectra of Scalar Potential Models of Inflation
- The Inflaton Effective Potential for General
- Final Thoughts on the Power Spectra of Scalar Potential Models
- Inflaton Effective Potential from Photons for General
- Coincident Massless, Minimally Coupled Scalar Correlators on General Cosmological Backgrounds
- From Non-trivial Geometries to Power Spectra and Vice Versa
- Explosive particle production in non-commutative inflation
- Inflaton Effective Potential from Fermions for General
- The Effect of Features on the Functional Form of the Scalar Power Spectrum
- Non-Gaussianity from Features
- Reheating with Effective Potentials