Speaker
Description
We construct posterior distributions of equations of state (EoS),
relevant to the studies of neutron stars (NSs), by applying Bayesian
approach to two different models. The EoSs are subjected to minimal
constraints which correspond to a few basic properties of nuclear
matter at the saturation density and the low density pure neutron
matter EoS obtained from a precise next-to-next-to-next-to-leading
order (N$^{3}$LO) calculation in chiral effective field theory. The tidal deformability and radius of neutron star over a wide range of mass are found to be strongly co-related with pressure of $\beta$-equilibrated matter as well as the symmetry energy at densities higher than the saturation($\rho_0$) density in a model independent manner. These correlations are employed to parametrized the pressure for $\beta$-equilibrium matter, around 2$\rho_0$, as a function of neutron star mass and the corresponding tidal deformability.The maximum mass of neutron star is also strongly correlated with pressure of $\beta$-equilibrated matter and symmetric nuclear matter at densities $\sim$ 4.5$\rho_0$. The combined effects of available bounds on the NS properties in constraining the EoS are also explored.
