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The recent measurement of the mass of neutron stars (PSR J1614 - 2230, PSRJ0348 + 0432, MSP J0740 + 6620) restricts the lower limit $\sim 2M_{\odot}$ ofthe maximum mass of such compact stars, making it possible for dense matter toexist in massive stars. The relativistic mean field theory with parameter setsFSUGold including Kaon condensation is used to describe the properties ofneutron stars in $\beta$ equilibrium. Through careful choice of the parameterof the $\sigma$-cut $c_{\sigma}$, we are able to produce a maximum mass neutronstar with Kaon condensation heavier than $2M_{\odot}$, and we find that theparameter $\Lambda_{\nu}$ of the $\rho-\omega$ interaction term in this modelhas a significant effect on $K^{-}$ condensation. In the case of using$\sigma$-cut scheme, $K^{-}$ condensation occurs only when the $\rho-\omega$interaction $\Lambda_{\nu}$ is switched off.

Kaon meson condensate in neutron star matter including hyperons