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From the very first multimessenger event of GW170817, clean robustconstraints can be obtained for the tidal deformabilities of the two starsinvolved in the merger, which provides us unique opportunity to study theequation of states (EOSs) of dense stellar matter. In this contribution, weemploy a model from the quark level, describing consistently a nucleon andmany-body nucleonic system from a quark potential. We check that our sets ofEOSs are consistent with available experimental and observational constraintsat both sub-nuclear saturation densities and higher densities. The agreementswith ab-initio calculations are also good. Especially, we tune the densitydependence of the symmetry energy (characterized by its slope at nuclearsaturation $L$) and study its influence on the tidal deformability. Theso-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 tothe uncertain crust-core matching, despite the good correlation between thesymmetry energy slope and the radius of the star.

Note on neutron star equation of state in the light of GW170817