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We study the hadron-quark hybrid equation of state (EOS) of compact-starmatter. The Nambu-Jona-Lasinio (NJL) local SU(3) model with vector-typeinteraction is used to describe the quark matter phase, while the relativisticmean field (RMF) theory with scalar-isovector $\delta$-meson effective fieldadopted to describe the hadronic matter phase. It is shown that the larger thevector coupling constant , the lower the threshold density for the appearanceof strange quarks. For a sufficiently small value of the vector couplingconstant, the functions of the mass dependence on the baryonic chemicalpotential have regions of ambiguity which leads to a phase transition innon-strange quark matter with an abrupt change in the baryon number density. Weshow that within the framework of the NJL model, the hypothesis on the absolutestability of strange quark matter is not realized. In order to describe thephase transition from hadronic matter to quark matter, the Maxwell'sconstruction is applied. It is shown that the greater the vector coupling, thegreater the stiffness of the EOS for quark matter and the phase transitionpressure. Our results indicate that the infinitesimal core of the quark phase,formed in the center of the neutron star, is stable.

Hadron-quark phase transition in the SU(3) local Nambu-Jona-Lasinio (NJL) model with vector interaction