Simulations with a tunable phase-transition parameter in neutron-star equations of state produce unique post-merger gravitational-wave peaks and link Δp to the prompt-collapse mass threshold, with Δp ≲ 0.04 implied for GW170817.
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Massless topological shells inside neutron stars produce non-monotonic shifts in f-mode frequencies and potentially detectable changes in gravitational-wave damping times and strains relative to standard models.
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Distinct Signatures of the Nature of Phase Transition in Binary Neutron Star Mergers
Simulations with a tunable phase-transition parameter in neutron-star equations of state produce unique post-merger gravitational-wave peaks and link Δp to the prompt-collapse mass threshold, with Δp ≲ 0.04 implied for GW170817.
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Topological Shell Structures in Neutron Stars: Effects on Equilibrium, Oscillations, and Gravitational-Wave Signatures
Massless topological shells inside neutron stars produce non-monotonic shifts in f-mode frequencies and potentially detectable changes in gravitational-wave damping times and strains relative to standard models.