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Theories beyond the standard model include a number of new particles some ofwhich might be light and weakly coupled to ordinary matter. Such particlesaffect equation of state of nuclear matter and can shift admissible masses ofneutron stars to higher values. The internal structure of neutron stars ismodified provided the ratio between coupling strength and mass squared of aweakly interacting light boson is above $g^2/\mu^2 \sim 25 ~\mathrm{GeV}^{-2}$.We provide limits on the couplings with the strange sector, which cannot beachieved from laboratory experiments analysis. When the couplings to the firstfamily of quarks is considered the limits imposed by the neutron stars are notmore stringent than the existing laboratory ones. The observations on neutronstars give evidence that equation of state of the $\beta$-equilibrated nuclearmatter is stiffer than expected from many-body theory of nuclei and nuclearmatter. A weakly interacting light vector boson coupled predominantly to thesecond family of the quarks can produce the required stiffening.

Constraints for weakly interacting light bosons from existence of massive neutron stars