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Time | Thursday, Mar 8 | Friday, Mar 9 |
---|---|---|

09.00 | K. Enqvist | K. Kajantie |

09.30 | S. Räsänen | E. Keski-Vakkuri |

10.00 | K. Kainulainen | H. Kurki-Suonio |

10.30 | Coffee | Coffee |

11.00 | M. Yamaguchi | D. Podolsky |

11.30 | D. Lyth | F. Vernizzi |

12.00 | ||

12.30 | Lunch & Free time for discussions | Lunch & Free time for discussions |

13.00 | ||

13.30 | ||

14.00 | N. Jokela | T. Mattsson |

14.30 | S. Kasuya | S. Kawai |

15.00 | T. Kanzaki | M. Kawasaki |

15.30 | T. Takayama | D. Grumiller |

16.00 | Coffee | Coffee |

16.30 | T. Takahashi | N. Sugiyama |

17.00 | K. Ichikawa | Y. Tanaka |

17.30 | M. Sloth | End |

18.00 | ||

... | ||

19.00 | Conference dinner |

One of the highlights of gauge/gravity duality is the prediction of the equation of state of strongly coupled supersymmetric Yang-Mills matter. We study how this duality could be extended from static to dynamic phenomena, to Y-M matter in ideal expansion. Planning to study spherical expansion in Minkowski space, a little bang, we end up with big bang, the flat FRW metric. Nevertheless, the result also applies for the little bang in the rest frame of the flow.

Primordial perturbations are supposed to originate during inflation, from the vacuum fluctuation of one or more bosonic fields. Non-gaussianity corresponds to a correlation between different Fourier components, generated by an interaction in the field theory describing the perturbations. Focussing on the curvature perturbation, we review the present situation in the standard scenario and in the curvaton scenario, and point to future directions of research.

I will explain how an inhomogeneous model of the universe can fit various cosmological observations without dark energy and accelerating expansion.

I discuss the possibility that the observed accelerated expansion of the universe could be explained by accounting for the effects of the inhomogeneities related to structure formation, without introducing a new matter component or modifying gravity. I demonstrate with an exact toy model how gravitational collapse induces accelerating expansion, and discuss how this mechanism could work in the real universe.

Using the gradient expansion approach, we formulate a nonlinear cosmological perturbation theory on super-horizon scales valid to $O(\epsilon^2)$, where $\epsilon$ is the expansion parameter associated with a spatial derivative. We consider the case of a single scalar field, and take into account not only scalar but also vector and tensor modes. We derive the general solution under the uniform-Hubble time-slicing. In doing so, we identify the scalar, vector and tensor degrees of freedom contained in the solution.

There will be a choice between a vegetarian/nonvegetarian menu. Thursday morning we will circulate a list, where we ask you to indicate your choice, and inform us of any food allergies. The conference dinner is free for registrants. |