  Three parameterizations DOPS1, DOPS2, and DOPS3 (named after the Department
of Physics Shimla) of the Relativistic Mean Field (RMF) model have been
proposed with the inclusion of all possible self and mixed interactions between
the scalar-isoscalar (\sigma), vector-isoscalar (\omega) and vector-isovector
(\rho) mesons up to quartic order. The generated parameter sets are in harmony
with the finite and bulk nuclear matter properties.
  A set of Equations of State (EOSs) composed of pure hadronic (nucleonic)
matter and nucleonic with quark matter (hybrid EOSs) for superdense
hadron-quark matter in \beta-equilibrium is obtained. The quark matter phase is
calculated by using the three-flavor Nambu-Jona-Lasinio (NJL) model. The
maximum mass of a non-rotating neutron star with DOPS1 parameterization is
found to be around 2.6 M$\odot$ for the pure nucleonic matter which satisfies
the recent gravitational wave analysis of GW190814 Abbott et al.,(2020) with
possible maximum mass constraint indicating that the secondary component of
GW190814 could be a non-rotating heaviest neutron star composed of pure
nucleonic matter. EOSs computed with the DOPS2 and DOPS3 parameterizations
satisfy the X-Ray observational data and the recent observations of GW170817
maximum mass constraint of a stable non-rotating neutron star in the range 2.01
\pm 0.04 - 2.16 \pm 0.03 M\odot and also in good agreement with constraints on
mass and radius measurement for PSR J0740+6620 (NICER) Riley et al., L27
(2021)}, Miller et al., (2021). The hybrid EOSs obtained with the NJL model
also satisfy astrophysical constraints on the maximum mass of a neutron star
from PSR J1614-2230 and Demorest et al., (2010) .We also present the results
for dimensionless tidal deformability, ${\Lambda}$ which are consistent with
the waveform models analysis of GW170817.
