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Non-Identical Neutron Star Twins
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The work of J. A. Wheeler in the mid 1960's showed that for smooth equations of state no stable stellar configurations with central densities above that corresponding to the limiting mass of ``neutron stars'' (in the generic sense) were stable against acoustical vibrational modes. A perturbation would cause any such star to collapse to a black hole or explode. Accordingly, there has been no reason to expect that a stable degenerate family of stars with higher density than the known white dwarfs and neutron stars might exist. We have found a class of exceptions corresponding to certain equations of state that describe a first order phase transition. We discuss how such a higher density family of stars could be formed in nature, and how the promising new exploration of oscillations in the X-ray brightness of accreting neutron stars might provide a means of identifying them. Our proof of the possible existence of a third family of degenerate stars is one of principle and rests on general principles like causality, microstability of matter and General Relativity.
Forward citations
Cited by 7 Pith papers
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How Neutron Star Radii Encode the Dense-Matter Equation of State and Hadron-Quark Transition
A Bayesian analysis of mock neutron star radius measurements shows that precision radii mainly constrain the symmetry-energy parameters L and Ksym and the quark transition density, while transition strength and quark ...
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Determining the minimal mass of a proto-neutron star with chirally constrained nuclear equations of state
For chirally constrained nuclear equations of state, the minimal proto-neutron star mass is about 0.62 solar masses with trapped neutrinos (YL=0.4, s=1) and about 0.22 solar masses after deleptonization (s=2).
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Quantifying the Information Gain from Future High-Precision Radius Measurements for Identifying Twin Neutron Stars
The paper claims a radius precision of ~0.2 km is enough to extract most Bayesian information for identifying twin neutron stars, but its own distinguishability and entropy analyses suggest notable gains remain down t...
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Constraints on the strength of first-order phase transition and its relation to nucleon mass
Using a parity doublet hadronic model, an NJL quark model, and integral causality constraints, the paper finds that the maximum allowed first-order phase-transition density jump in neutron-star matter decreases as the...
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Probing Neutron Star Interiors and the Properties of Cold Ultra-dense Matter with the SKAO
SKAO's sensitivity, surveys and sub-arraying will deliver tighter NS mass, MoI, spin, glitch and precession constraints that, with X-ray and GW data, probe cold ultra-dense matter.
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Nuclear Physics of Binary Neutron Star Mergers
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.
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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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