PIRSA:13040128

Video URL

https://pirsa.org/13040128

Transporting non-Gaussianity from sub- to super- horizon scales

Mulryne, D. (2013). Transporting non-Gaussianity from sub- to super- horizon scales. Perimeter Institute for Theoretical Physics. https://pirsa.org/13040128

Mulryne, David. Transporting non-Gaussianity from sub- to super- horizon scales. Perimeter Institute for Theoretical Physics, Apr. 30, 2013, https://pirsa.org/13040128 

          @misc{ scivideos_PIRSA:13040128,
            doi = {10.48660/13040128},
            url = {https://pirsa.org/13040128},
            author = {Mulryne, David},
            keywords = {Cosmology},
            language = {en},
            title = {Transporting non-Gaussianity from sub- to super- horizon scales},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2013},
            month = {apr},
            note = {PIRSA:13040128 see, \url{https://scivideos.org/pirsa/13040128}}
          }

David Mulryne Queen Mary University of London

Talk numberPIRSA:13040128
DOI10.48660/13040128
Source RepositoryPIRSA
Collection
Talk Type Scientific Series
Subject

Abstract

The non-Gaussian statistics of the primordial density perturbation have become a key test of the inflationary scenario of the very early universe. Currently many techniques are used to calculate the non-Gaussian signatures of a given model of inflation. In particular, simple super-horizon techniques such as the deltaN formalism are often used for models with more than one field, while more technical field theory techniques, referred to as the In-In formalism, are typically used for models where the quantum sub-horizon evolution is important. Recently we have been developing an alternative point of view, called the transport approach. This framework highlights the connections between these other techniques and unifies them. Moreover, since it reduces the problem of calculating the statistics to that of solving a set of coupled ODEs, numerical implementations of the system are extremely simple.