Speaker
Description
Modern formulations of nuclear forces, such as pionless or chiral effective field theory, are typically based on a perturbative approach. Such interactions are then often employed by state-of-the-art nuclear many-body techniques (such as quantum Monte Carlo) which are non-perturbative in nature. The equation of state of a compact star is thus the result of this interplay of perturbative nuclear force and non-perturbative many-body method. Despite the centrality of this question to nuclear ab initio predictions, the perturbative use of nuclear interactions as input is still in its infancy (i.e., limited to first order). In this talk I will report on our recent work fusing non-perturbative approaches and second-order perturbation theory. Results will build up to the order-by-order convergence of chiral Effective Field Theory interactions for pure neutron matter.
