PIRSA:16090041

Converting entropy to curvature perturbations after a cosmic bounce

Fertig, A. (2016). Converting entropy to curvature perturbations after a cosmic bounce . Perimeter Institute. https://pirsa.org/16090041

Fertig, Angelika. Converting entropy to curvature perturbations after a cosmic bounce . Perimeter Institute, Sep. 06, 2016, https://pirsa.org/16090041 

          @misc{ pirsa_PIRSA:16090041,
            doi = {10.48660/16090041},
            url = {https://pirsa.org/16090041},
            author = {Fertig, Angelika},
            keywords = {Cosmology},
            language = {en},
            title = {Converting entropy to curvature perturbations after a cosmic bounce },
            publisher = {Perimeter Institute},
            year = {2016},
            month = {sep},
            note = {PIRSA:16090041 see, \url{https://pirsa.org}}
          }

Angelika Fertig

TotalEnergies (France)

Talk number
PIRSA:16090041
Collection
Talk Type
Subject
Abstract

In this talk, I will show how entropy perturbations created during a contracting phase and converted into adiabatic/curvature perturbations after a bounce form the dominant contribution to the observed temperature fluctuations in the CMB.
In [arXiv:1607.05663] we have studied two-field bouncing cosmologies in which primordial perturbations are created in either an ekpyrotic or a matter-dominated contraction phase. We then used a non-singular ghost condensate bounce model to follow the perturbations through the bounce into the expanding phase of the universe. In contrast to the adiabatic perturbations, which on large scales are conserved across the bounce, entropy perturbations can grow significantly during the bounce phase. If they are converted into adiabatic/curvature perturbations after the bounce, they typically form the dominant contribution to the observed temperature fluctuations in the microwave background, which can have several beneficial implications. For ekpyrotic models, this mechanism loosens the constraints on the amplitude of the ekpyrotic potential while naturally suppressing the intrinsic amount of non-Gaussianity. For matter bounce models, the mechanism amplifies the scalar perturbations compared to the associated primordial gravitational waves with the consequence that the tensor-to-scalar ratio is typically reduced by an order of magnitude or so, bringing it close to current observational bounds.