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We investigate the influence of repulsive vector interactions and colorsuperconductivity on the structure of neutron stars using an extended versionof the field correlator method (FCM) for the description of quark matter. Thehybrid equation of state is constructed using the Maxwell description, whichassumes a sharp hadron-quark phase transition. The equation of state ofhadronic matter is computed for a density-dependent relativistic lagrangiantreated in the mean-field approximation, with parameters given by the SW4Lnuclear model. This model described the interactions among baryons in terms of$\sigma, \omega, \rho, \sigma^*$, and $\phi$ mesons. Quark matter is assumed tobe in either the CFL or the 2SC+s color superconducting phase. The possibilityof sequential (hadron-quark, quark-quark) transitions in ultra-dense matter isinvestigated. Observed data related to massive pulsars, gravitational-waveevents, and NICER are used to constrain the parameters of the extended FCMmodel. The successful equations of state are used to explore the mass-radiusrelationship, radii, and tidal deformabilities of hybrid stars. A special focuslies on investigating consequences that slow or fast conversions ofquark-hadron matter have on the stability and the mass-radius relationship ofhybrid stars. We find that if slow conversion should occur, a new branch ofstable massive stars would exist whose members have radii that are up to 1.5~kmsmaller than those of conventional neutron stars of the same mass. Such objectscould be possible candidates for the stellar high-mass object of the GW190425binary system.

Hybrid stars with color superconducting cores in an extended FCM model