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Neutron stars with small radii -- the role of delta resonances
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Recent neutron star observations suggest that the masses and radii of neutron stars may be smaller than previously considered, which would disfavor a purely nucleonic equation of state. In our model, we use a the flavor SU(3) sigma model that includes delta resonances and hyperons in the equation of state. We find that if the coupling of the delta resonances to the vector mesons is slightly smaller than that of the nucleons, we can reproduce both the measured mass-radius relationship and the extrapolated equation of state.
Forward citations
Cited by 3 Pith papers
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Astrophysical Constraints on Hadron--Quark Crossover in Hybrid Neutron Stars
A Bayesian analysis of smooth hadron-quark crossover neutron stars using NICER and GW170817 data favors a broad, high-density mixed transition, disfavors pure quark cores, and makes a neutron-star interpretation of GW...
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Exploring the impact of $\Delta$-isobars on Neutron Star
Adding delta isobars with adjustable meson couplings can shift their appearance density below lambda hyperons and change the predicted radius of a 1.4 solar mass neutron star by up to about 1.7 km.
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The equation of state for neutron stars
A textbook-style review of the neutron-star equation of state covering the models, experimental and observational constraints, and open questions, with no new result claimed or derived.
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