The density perturbation power spectrum to second-order corrections in the slow-roll expansion
By E. Stewart, Jinagbin Gong. 2001
213 citations recorded by the source corpus.
Abstract We set up a formalism that can be used to calculate the power spectrum of the curvature perturbations produced during inflation up to arbitrary order in the slow-roll expansion, and explicitly calculate the power spectrum and spectral index up to second-order corrections.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/cc1323c0961be089404bf1d5b164b40c52a51dfb
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In Astronomy and Astrophysics
- Jérôme Martin
- C. Ringeval
- Robert Brandenberger
- R. Easther
- Peter Adshead
- J. Pritchard
- Abraham Loeb
- U. Danielsson
Citations in the corpus
- Primordial non-Gaussianities in single-field inflation (2005, unknown): “However, in any effective theory it is to be expected that terms containing higher derivatives will be suppressed by powers of the ultraviolet cutoff scale.”
- Inflation after WMAP3: confronting the slow-roll and exact power spectra with CMB data (2006, methodology): “ terms of Bessel functions are no longer valid. It is therefore necessary to use more sophisticated methods either based on the WKB approximation [46, 47, 48, 49] and/or on the Green function methods [50, 51]. The latter method has been used in several works [50, 44] to derive the coefficients ai and ”