  From the very first multimessenger event of GW170817, clean robust
constraints can be obtained for the tidal deformabilities of the two stars
involved in the merger, which provides us unique opportunity to study the
equation of states (EOSs) of dense stellar matter. In this contribution, we
employ a model from the quark level, describing consistently a nucleon and
many-body nucleonic system from a quark potential. We check that our sets of
EOSs are consistent with available experimental and observational constraints
at both sub-nuclear saturation densities and higher densities. The agreements
with ab-initio calculations are also good. Especially, we tune the density
dependence of the symmetry energy (characterized by its slope at nuclear
saturation $L$) and study its influence on the tidal deformability. The
so-called $QMF18$ EOS is named after the case of $L=40~\rm MeV$, and it gives
$M_{\rm TOV} =2.08~M_\odot$ and $R= 11.77~\rm km$, $\Lambda=331$ for a
$1.4\,M_\odot$ star. The tidal signals are demonstrated to be insensitive to
the uncertain crust-core matching, despite the good correlation between the
symmetry energy slope and the radius of the star.
