Neutron stars with a crossover equation of state

Abstract

The question of whether quark matter exists in neutron stars is a long standing one. Generally one finds that a first order phase transition from baryons to quarks softens the equation of state so much that the star would collapse into a black hole. We consider a crossover equation of state, similar to the crossover that is found in lattice QCD studies at finite temperature and zero or small baryon chemical potentials. We find that with reasonable parameters it may be possible to support neutron stars up to about 2.2 solar masses. In that case 1 to 10% of the pressure would be contributed by quark matter in the central core of the highest mass stars.

arXiv comment4 pages, 5 figures

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• Quasi-normal g-modes of neutron stars with quarks
• Impact of massive neutron star radii on the nature of phase transitions in dense matter
• Effect of color superconductivity on the mass of hybrid neutron stars in an effective model with pQCD asymptotics
• Novel neutron decay mode inside neutron stars
• Hybrid star phenomenology from the properties of the special point
• Topology and emergent symmetries in dense compact star matter
• Scale symmetry and composition of compact star matter
• Simulating neutron stars with a flexible enthalpy-based equation of state parametrization in SpECTRE
• The sound speed and core of massive compact stars: A manifestation of hadron-quark duality
• Fundamental-mode eigenfrequencies of neutral and charged twin neutron stars