Estimating the values and variations of neutron star observables by dense nuclear matter properties

Recent NICER observation data on PSR J0030+0451 has recently added a unique mass-radius constraint on the properties of the superdense nuclear matter existing in the interior of compact stars. Such a macroscopic data restrict further the microscopical models, elementary interactions, and their parameters, however, with reasonable margin because of the masquarade problem. Here our goal is to identify the origin and quantify the magnitude of the theoretical uncertainties of the nuclear matter models. A detailed study on the effect of different interaction terms and the nuclear parameter values in the Lagrangian of the extended $σ$-$ω$ model is presented here. The equation of state was inserted to the Tolman--Oppenheimer--Volkoff equation and observable parameters of the neutron star were calculated. We identified, that the optimal Landau effective mass is the most relevant physical parameter modifying the macroscopic observable values. Moreover, the compressibility and symmetry energy terms just generate one-one order of magnitude smaller effect to this, respectively. We calculated the linear relations between the maximal mass of a compact star and these microscopic nuclear parameter values within the physical relevant parameters range. Based on the mass observational data we estimated the magnitude of the radii of PSR J1614-2230, PSR J0348+0432, and PSR J0740+6620 including theoretical uncertainties arising from the models' interaction terms and their parameter values choices.