Abstract: Neutron stars (NS) are cosmic laboratories that allow us to probe the fundamental aspects of matter under the most extreme conditions, bridging gaps across various domains of physics. This seminar provides a detailed examination of the cold, dense baryonic equation of state (EOS) that controls these mysterious objects. It will explore the limitations imposed by chiral effective field theory at low densities, as well as perturbative quantum chromodynamics (QCD) at very high densities, in addition to observational constraints from neutron stars. Despite recent advances through observational milestones by Neutron Star Interior Composition Explorer (NICER) and LIGO-Virgo, the neutron star core composition remains elusive, with potential scenarios ranging from only nucleonic matter to deconfined quark matter. This talk will outline recent innovations in modelling the EOS, also highlighting the roles of Bayesian neural networks (BNNs) in decoding the observable properties of neutron stars to shed light on their internal composition. These studies guide future observations such as those by the Einstein Telescope (ET) to pinpoint binary systems that could be key to decoding the internal structure of neutron stars. The seminar will also discuss the significance of the tidal deformability measurements from Gravitational Waves (GW) of binary NS and the role of nuclear symmetry energy in constraining the EOS. In conclusion, the presence of dark matter within NS will also be examined, along with the future exploration of different machine learning methods to pinpoint its existence in NS.

Meeting ID: 930 0327 5527
Passcode: 536663