Hydrodynamics of the simple exclusion process in random environment: a mild solution approach.
Federico Sau, IST Austria.
In this talk, we discuss an alternative point of view, initiated by the works of Nagy (2001) and Faggionato (2007), on the hydrodynamic limit of the exclusion process. We show how this method based on duality and a mild solution representation of the empirical measures carries over to the case of random environment - both static and dynamic. In conclusion, we discuss some recent refinements of this method which allow, for instance, to obtain tightness of the sequence of empirical measures.
Joint work with S. Floreani (TU Delft), F. Redig (TU Delft) and E. Saada (Paris V Descartes).
Finite order period integrals in normal crossing K3 degenerations.
Helge Ruddat, Gutenberg University.
I am presenting a new technique to compute period integrals of degenerating Calabi-Yau manifolds. In the K3 case, the formula can be used to study the Picard group of nearby fibres. In general, the technique leads to canonical parametrizations of degenerating families at the boundary of the moduli space. The result enters ongoing work by Gross-Hacking-Keel-Siebert on a modular compactification of the family of g-polarized K3 surfaces. This is joint with Bernd Siebert.
Generalized Gibbs Ensemble and KdV charges in 2d CFTs.
Simon Ross, Durham University.
2d CFTs have an infinite set of commuting conserved charges, known as the quantum KdV charges. There is a generalised Gibbs ensemble for these theories where we turn on chemical potentials for these charges. I will describe some partial results on calculating this partition function, both in the limit of large charges and perturbatively in the chemical potentials.
Global Existence for the N Body Euler-Poisson System.
Shrish Parmeshwar, King's College London.
We discuss the problem of multiple expanding Newtonian stars acting under gravitational attraction. In particular, we will investigate whether one can find a class of initial positions and velocities for each star such that these expanding stars never touch. To do this, we make use of a scaling property present in the compressible Euler system, as well as a careful analysis of how the gravitational interaction between stars affects their dynamics.
To be announced.
Jorge V. Rocha, ICCUB.