Abstract
We investigate the effects of the light vector U boson that couples weakly to nucleons in relativistic mean-field models on the equation of state and subsequently the consequence in neutron stars. It is analyzed that the U boson can lead to a much clearer rise of the neutron star maximum mass in models with the much softer equation of state. The inclusion of the U boson may thus allow the existence of the non-nucleonic degrees of freedom in the interior of large mass neutron stars initiated with the favorably soft EOS of normal nuclear matter. In addition, the sensitive role of the U boson in the neutron star radius and its relation to the test of the non-Newtonian gravity that is herein addressed by the light U boson are discussed.
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