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We investigate the effects of the light vector U-boson that couples weakly tonucleons in relativistic mean-field models on the equation of state andsubsequently the consequence in neutron stars. It is analyzed that the U-bosoncan lead to a much clearer rise of the neutron star maximum mass in models withthe much softer equation of state. The inclusion of the U-boson may thus allowthe existence of the non-nucleonic degrees of freedom in the interior of largemass neutron stars initiated with the favorably soft EOS of normal nuclearmatter. In addition, the sensitive role of the U-boson in the neutron starradius and its relation to the test of the non-Newtonian gravity that is hereinaddressed by the light U-boson are discussed.

Effects of a weakly interacting light U boson on the nuclear equation of state and properties of neutron stars in relativistic models