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 QMF 18 EOS is named after the case of L = 40 ~ { } MeV , and it gives M _ { TOV } = 2.08 ~ { } M _ { \odot } and R = 11.77 ~ { } km , \Lambda = 331 for a 1.4 M _ { \odot } star .
The tidal signals are demonstrated to be insensitive to the uncertainty on the crust-core matching , despite the good correlation between the symmetry energy slope and the radius of the star .