  The properties of hadron-quark hybrid stars are studied when the quark phase
is described in terms of a local SU(3) Nambu--Jona-Lasinio (NJL) model taking
into account the contribution of the vector and axial-vector interaction
between the quarks, and the hadronic phase, in the relativistic mean field
(RMF) model. For different values of the vector coupling constant $G_V$, the
equations of state of the quark matter are calculated and the parameters of the
hadron-quark phase transition are determined under the assumption that the
phase transition takes place in accordance with Maxwell's construction. It is
shown that for a larger vector coupling constant, the equation of state of the
quark matter will be "stiffer" and the coexistence pressure $P_0$ of the phases
will be greater. Using the resulting hybrid equations of state, the TOV
equations are integrated numerically and the mass and radius of the compact
star are determined for different values of the central pressure $P_c$. It is
shown that when $G_V$ is larger, the maximum mass of the compact star will be
larger and thereby, the radius of the configuration with maximum mass will be
smaller. Questions of the stability of hybrid stars are also discussed. It is
shown that in terms of the model examined here, for all values of the vector
coupling constant, a hybrid star with an infinitely small quark core is stable.
These results are compared with recent measurements of the mass and radius of
the pulsars PSR J0030+0451 and PSR J0740+6620, carried out at the International
Space Station with the NASA's Neutron star Interior Composition Explorer
(NICER) X-ray telescope. A comparison of the theoretical results with
observational data does not exclude the possibility of quark deconfinement in
the interiors of compact stars.
