Natureza da transição de fase quark-hádron e consequências para a estrutura estelar

Abstract

Neutron stars are the second most dense objects in the universe (only less dense than black holes) and have a relatively low temperature. Because of these features, neutron star matter lies in a poorly understood region of the QCD phase diagram. Neutron stars can work as laboratories for the study of cold and dense matter.In this work, we used the MFTQCD (Mean-Field Theory of Quantum Chromodynamics) and we obtained the mass-radius diagram and the tidal deformability. Comparing these results with the experimental data, we conclude that the MFTQCD remains a good model to describe the properties of neutron stars; however, the parameter window is now narrower. Next, we studied the impact of the nature of the phase transition on neutron star properties. We used an equation of state which combines hadronic matter and quark matter. We control the smoothness of the quark-hadron transition by varying the free parameter ρ c . Our results indicate that a sharp phase transition is more compatible with experimental data.