Up-down quark stars in the two-families scenario yield tidal deformabilities compatible with GW170817, constraining the effective bag constant to approximately 50 MeV/fm^3.
nEoS: Neutron Star Equation of State from hadron physics alone
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abstract
We contribute a publicly available set of tables and code to provide Equations of State (EoS) for matter at neutron star densities. Our EoSes are constrained only by input from hadron physics and fundamental principles, without feedback from neutron star observations, and so without relying on General Relativity. They can therefore be used to test General Relativity itself, as well as modified gravity theories, with neutron star observables, without logical circularity. We have adapted state of the art results from NN chiral potentials for the low--density limit, pQCD results for the asymptotically high-density EoS, and use monotonicity and causality as the only restrictions for intermediate densities, for the EoS sets to remain as model-independent as is feasible today.
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Probing up-down quark matter via gravitational waves
Up-down quark stars in the two-families scenario yield tidal deformabilities compatible with GW170817, constraining the effective bag constant to approximately 50 MeV/fm^3.