Equation of State of Nuclear Matter with Gaussian Processes

Abstract

In this work we employ a Gaussian Processes method to obtain a non-parametric description of the Equation of State (EoS) of cold dense matter that allows for rapid calculations and gives an estimation of the uncertainty of the theoretical model and related observables. The calculations are based on results derived in a Bruckner-Hartree-Fock approach. The non-parametric EoS is then used to study asymmetric β-stable neutron star matter, obtaining its composition, the pressure and the energy density at different baryonic densities. By solving the Tolman- Oppenheimer-Volkoff equations, we also determine the stellar structure parameters. Our results for the non-parametric EoS are consistent with those obtained with a traditional power-law fit to the data.