Structural Properties of Rotating Hybrid Compact Stars with
  Color-Flavour-Locked Quarks Matter core and its Tidal Deformability
  We investigate the possible sequels, for the hybrid compact stars consisting
of nucleons, hyperons and three flavour color-flavor-locked quarks phase under
global neutrality and chemical equilibrium conditions. The hadron equations of
state are computed within the framework of energy density functionals based on
the relativistic mean field theory by employing two different model
parameterizations. The quarks matter phase of equation of state is computed by
using Quarks Quasiparticle model derived from a non-relativistic energy
density-functional approach. A plausible set of hybrid equations of state for
superdense hadron-quarks matter is obtained and, which satisfies the
constraints provided by bulk nuclear matter, the observational data of
frequencies and maximum Gravitational mass 2$M_\odot$ with their extracted
radii, Keplerian limits, secular axisymmetric instability and limits of tidal
deformabilities from GW170817 binary neutron stars (BNS) merger. We obtained
structural properties of nonrotating and rotating compact stars, the
evolutionary sequences with constant baryonic mass star spinning down by
electromagnetic and gravitational radiations and, discuss the issues relating
to phase transition from hadrons to quarks matter phase. The internal structure
of rotating star with observed spin down frequencies, exhibiting shrinkage of
soft quarks core of compact stars are discussed for constant baryonic mass. We
present the theoretically computed limits of radii for the spin down
configurations of hybrid stars corresponding to the recently observed
millisecond pulsars. We also present and discuss the calculated results for
tidal deformability, $\Lambda$ and tidal parameters $\Lambda_1$, $\Lambda_2$ of
non spining hybrid star which are consistent with the waveform model analysis
of GW170817 BNS.
