  The concept of quarkyonic matter presents a promising alternative to the
conventional models used to describe high-density matter and provides a more
nuanced and detailed understanding of the properties of matter under extreme
conditions that exist in astrophysical bodies. The aim of this study is to
showcase the effectiveness of utilizing the quarkyonic model, in combination
with the relativistic mean-field formalism, to parameterize the equation of
state at high densities. Through this approach, we intend to investigate and
gain insights into various fundamental properties of a static neutron star,
such as its compositional ingredients, speed of sound, mass-radius profile, and
tidal deformability. The obtained results revealed that the quarkyonic matter
equation of state (EOS) is capable of producing a heavy neutron star with the
mass range of $\sim$ $2.8 M_\odot$. The results of our inquiry have
demonstrated that the EOS for quarkyonic matter not only yields a neutron star
with a significantly high mass but also showcases a remarkable degree of
coherence with the conformal limit of the speed of sound originating from
deconfined QCD matter. Furthermore, we have observed that the tidal
deformability of the neutron star, corresponding to the EOSs of quarkyonic
matter, is in excellent agreement with the observational constraints derived
from the GW170817 and GW190425 events. This finding implies that the quarkyonic
model is capable of forecasting the behavior of neutron stars associated with
binary merger systems. This aspect has been meticulously scrutinized in terms
of merger time, gravitational wave signatures, and collapse times using
numerical relativity simulations.
