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The low density nuclear matter equation of state is strongly constrained bynuclear properties, however, for constraining the high density equation ofstate it is necessary to resort to indirect information obtained from theobservation of neutron stars, compact objects that may have a central densityseveral times nuclear matter saturation density, $n_0$. Taking a meta-modellingapproach to generate a huge set of equation of state that satisfy nuclearmatter properties close to $n_0$ and that do not contain a first order phasetransition, the possibility of constraining the high density equation of statewas investigated. The entire information obtained from the GW170817 event forthe probability distribution of $\tilde{\Lambda}$ was used to make aprobabilistic inference of the EOS, which goes beyond the constraints imposedby nuclear matter properties. Nuclear matter properties close to saturation,below $2n_0$, do not allow us to distinguish between equations of state thatpredict different neutron star (NS) maximum masses. This is, however, not trueif the equation of state is constrained at low densities by the tidaldeformability of the NS merger associated to GW170817. Above $3n_0$,differences may be large, for both approaches, and, in particular, the pressureand speed of sound of the sets studied do not overlap, showing that theknowledge of the NS maximum mass may give important information on the highdensity EOS. Narrowing the maximum mass uncertainty interval will have asizeable effect on constraining the high density EOS.

Constraints on high density equation of state from maximum neutron star mass