  We study the equation of state of dense baryon matter within the relativistic
mean-field model, and we include ${\Delta}$(1232) isobars into IUFSU model with
hyperons and consider the possibility of kaon meson condensation. We find that
it is necessary to consider the $\Delta$ resonance state inside the massive
neutron star. The critical density of Kaon mesons and hyperons is shifted to a
higher density region, in this respect an early appearance of $\Delta$
resonances is crucial to guarantee the stability of the branch of hyperonized
star with the difference of the coupling parameter $x_{\sigma \Delta}$
constrained based on the QCD rules in nuclear matter. The $\Delta$ resonance
produces a softer equation of state in the low density region, which makes the
tidal deformability and radius consistent with the observation of GW170817. As
the addition of new degrees of freedom will lead to a softening of the equation
of state, the ${\sigma}$-cut scheme, which states the decrease of neutron star
mass can be lowered if one assumes a limited decrease of the ${\sigma}$-meson
strength at ${\rho_B}$($\rho_B > \rho_0$), finally we get a maximum mass
neutron star with $\Delta$ resonance heavier than 2$M_{\odot}$.
