Speaker
Description
Neutron star astrophysical observables provide a unique insight into the physics of dense matter. The famous binary neutron star merger GW170817 has particularly provided constraints on the equation of state of dense matter, revealing its softening in the core of neutron stars. Such insight is out of the reach of nuclear theory because of the non-perturbative nature of strong-interaction, and also inexplorable in nuclear physics laboratory experiments. I present the new semi-agnostic approach for equation of state constructions built for the purpose of dense matter Bayesian inference. I discuss the inference of not only the equation of state, but also of key nuclear empirical parameters that are of particular interest for nuclear physicists, and show that such inference has its limit, even in the context of extremely precise detections.