Research Projects

The nuclear equation of state (EoS) is a crucial component in studying the properties of neutron stars. There are various methods to parameterize realistic EoS models, including piecewise polytropic, relativistic mean field model, and chiral model EoS. The task of constraining the EoS and extracting correlations between NS observables and nuclear matter parameters near the nuclear saturation density is a joint effort between astrophysics and nuclear physics. A recently proposed meta-modeling for the nuclear EoS does this, focusing on the state-of-the-art knowledge of nuclear matter based on nuclear experiments. Despite some papers claiming no physical correlations exist among different empirical parameters, some studies show a strong correlation between the symmetry slope parameter and the tidal deformability of a 1.4 Msolar star. The aim is to disentangle these two aspects with detailed calculations, aiming to construct a non-parametric equation of state for the neutron star interior. This involves starting with piecewise polytrope EoS and moving on to density-dependent relativistic mean field model. The coefficients are used to extract local information from different nuclear models around the saturation density. The project aims to enhance our understanding of fundamental properties of neutron stars and help pinpoint the equation of state of dense matter relevant to compact stars. High-performance computing and parallel processing will be used, and young researchers will be trained to apply Bayesian techniques and machine learning, which could be useful in broader research and development areas.