for the case of APR and SLY4 EOSs. For the TM1 and NL3 EOSs, transition from nuclear matter to the CFL quark matter proceeds via 2SC phase at intermediate densities. For the BSR10 EOS, nuclear matter to CFL quark matter phase transition proceeds via 2SC phase only for G$_{D}$ = 1 . 2 G$_{S}$ with G$_{V}$ = 0. We see from these figures that the pressure, at which the tra nsition from the nuclear to quark matter occurs, decreases with increasing G$_{D}$ or decreasing G$_{V}$ . For instance, pressure at the phase transition reduces almost by a factor of two with increase in G$_{D}$ from 1 . 1 G$_{S}$ to 1 . 2 G$_{S}$ . The solid circles on the various EOSs for the nuclear matter indicate the values of P$_{1}$$_{.}$$_{4}$ which is the pressure at the center of the neutron star with the canonical mass (1 . 4 $^{M}$⊙ ). The values of transition pressure is close to that of P$_{1}$$_{.}$$_{4}$ for the cases plotted in the lower and the upper panels of Figs. 2 and 3, respectively. For the completeness, in the right panels of Figs. 2 and 3, we display the plots for the pressure as a function of the baryon density for the case of APR, BSR10 and NL3 EOSs. The phase transition to the quark matter is computed by a Maxwell construction. We construct the equilibrium sequences of the non-rotating and rotating compact stars using the EOSs obtained in the last section. These EOSs correspond to the nuclear matter at lower densities and the CSQM in the 2SC or CFL phase at higher densities as shown in Figs. 2 and 3. The nuclear matter EOSs are taken from the published literature as summarized in Table I. The EOSs for the CSQM are computed within the NJL model for di ff erent values of the scalar diquark coupling strength G$_{D}$ and the vector current coupling strength G$_{V}$ . The other parameters of the model are determined by fit to some of the observables of the vacuum QCD.The various EOSs as obtained in the present work can be completely specified by (i) the sourcefor the nuclear matter EOS as listed in Table I and (ii) the values of G$_{D}$ and G$_{V}$ used in computing the EOS of the CSQM within the NJL model. The properties of spherically symmetric non-rotating and axially symmetric rotating compact stars are obtained by solving the Einstein’s equations in 1D and 2D, respectively. The numerical computations are performed by using RNS code written by Stergioulas and Friedman [42]. The equilibrium sequence of compact stars for a given EOS is obtained by varying the central energy density ϵ$_{c}$ . For the stable configuration, where, M is the gravitational mass of the non-rotating compact star. The equilibrium sequences for the non-rotating compact stars resulting from our EOSs are plotted as mass versus radius in 6 III. HYBRID STARS WITH CSQM CORE ∂ M ∂ϵ$_{c}$ ⩾ 0 , (13)