  Properties of neutron stars in GW170817 are investigated using different
equations of state (EoS) involving nucleons, $\Lambda$ hyperons, quarks
resulting in $2M_{\odot}$ neutron stars. This calculation is performed using
the same EoS for merger components and for low spin prior case. It is found
from the computations of tidal deformability parameters that soft to moderately
stiff equations of state are allowed by the 50$\%$ and 90$\%$ credible regions
obtained from the gravitational wave observation of binary neutron star merger
GW170817, whereas the stiffest hadron-quark EoS which lies above the upper
90$\%$ limit, is ruled out. A correlation among the tidal deformabilities and
masses is found to exist as already predicted. Furthermore moments of inertia
and quadrupole moments of merger components of GW170817 are estimated.
