2009/04/30 by Kazunori Kohri, David H. Lyth, César A. Valenzuela-Toledo +1 · 63 citations
Mathematics · Physics and Astronomy · #Black Holes and Theoretical Physics #Chaotic #Cosmological perturbation theory #Cosmology and Gravitation Theories #Curvature #Galaxies: Formation, Evolution, Phenomena #Gaussian #Inflation (cosmology) #Mathematical physics #Mathematics #Non-Gaussianity #Perturbation (astronomy) #Physics #Pure mathematics #Quadratic equation #Quantum mechanics #Quartic function #Theoretical physics #astro-ph.CO #hep-ph #hep-th
paper · pdf · doi:10.1088/1475-7516/2010/02/023
published in Journal of Cosmology and Astroparticle Physics 2010(02), 023 (Institute of Physics) · The discussion around Eqs. (100) and (101) corrected and clarified (v4), Added new insights into (i) the status of the box size upon which loop contributions depend and (ii) the relevance for massless preheating of the numerical simulation of Bond et al. (v3) This paper is dedicated to the memory of Lev Kofman who died on 12th November 2009
openalex publication_date 2010/02/15 · arxiv created 2010/08/11 · arxiv updated 2011/03/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
The perturbation of a light field might affect preheating and hence generate a contribution to the spectrum and non-gaussianity of the curvature perturbation ζ. The field might appear directly in the preheating model (curvaton-type preheating) or indirectly through its effect on a mass or coupling (modulated preheating). We give general expressions for ζ based on the δ N formula, and apply them to the cases of quadratic and quartic chaotic inflation. For the quadratic case, curvaton-type preheating is ineffective in contributing to ζ, but modulated preheating can be effective. For quartic inflation, curvaton-type preheating may be effective but the usual δ N formalism has to be modified. We see under what circumstances the recent numerical simulation of Bond et al. [ 0903.3407 ] may be enough to provide a rough estimate for this case.