Bayesian inference on the equation of state from neutron stars properties

this paper, we apply Bayesian inference to constrain the nuclear equation of state parameters by using properties of neutron stars, including the maximum neutron star mass, radius, tidal deformability at 1.4 times the solar mass, and speed sound. When the polytrope EOS parameter y is fixed at 2.9 and above four astronomical observations are simultaneously used, the mean values and uncertainties of the nuclear matter parameters derived from standard Skyrme interactions are follows: incompressibility K 0 = 243.4 +/- 22.0 MeV, symmetry energy coefficient S 0 = 29.3 +/- 2.9 MeV, the slope of symmetry energy L = 74.4 +/- 14.8 MeV, the isoscalar effective mass m & lowast;s/m = 0.79 +/- 0.13, and a quantity related to effective mass splitting fI = 0.08 +/- 0.30 (when fI > 0, this implies that the effective mass of neutrons is less than that of protons). When considering the uncertainty of y in the range of 2.45-2.9, we found that K 0 increased by 11%, S 0 decreased by 2%, decreased by 20%, m & lowast;s/m decreased by 4%, and the averaged value of fI reduced by 88%. Particularly, if constraints are based solely on neutron star masses less than 2.05 M circle dot , the preferred effective Skyrme interactions exhibit a neutron effective mass greater than the proton effective mass, i.e., fI < 0. The inverse sign of the constrained fI implies that reducing the uncertainties of the effective Skyrme interaction parameters needs combination analysis with heavy-ion collisions in future studies.