Speaker
Description
The asymmetron dark energy model is an extension of the symmetron that aspires to resolve some of the cosmological tensions by allowing for a late-time, stochastic and large-scale spatial variation of the effective gravitational constant, in addition to the environmental variation due to screening. Whether this model actually manages to do so is complicated as it relates to questions of stability of the domain walls, how the field configuration traces the cold dark matter structure and the resultant domain sizes. To model this self-consistently requires resolving a large range in temporal and spatial scales, which we have set out to do here. I will show some of our convergence results on the field configurations, and make comments on features of the fully non-linear and dynamic model that we have gained access to. I will make comparisons between the symmetron and the asymmetron.
