Kaon meson condensate in neutron star matter including hyperons

Understand

The recent measurement of the mass of neutron stars (PSR J1614 - 2230, PSR J0348 + 0432, MSP J0740 + 6620) restricts the lower limit $\sim 2M_{\odot}$ of the maximum mass of such compact stars, making it possible for dense matter to exist in massive stars.

• The relativistic mean field theory with parameter sets FSUGold including Kaon condensation is used to describe the properties of neutron stars in $\beta$ equilibrium.
• Through careful choice of the parameter of the $\sigma$-cut $c_{\sigma}$, we are able to produce a maximum mass neutron star with Kaon condensation heavier than $2M_{\odot}$, and we find that the parameter $\Lambda_{\nu}$ of the $\rho-\omega$ interaction term in this model has 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.