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.
Barotropic thin shells with linear EOS as models of stars and circumstellar shells in general relativity
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abstract
The spherically symmetric thin shells of the barotropic fluids with the linear equation of state are considered within the frameworks of general relativity. We study several aspects of the shells as completely relativistic models of stars, first of all the neutron stars and white dwarfs, and circumstellar shells. The exact equations of motion of the shells are obtained. Also we calculate the parameters of the equilibrium configurations, including the radii of static shells. Finally, we study the stability of the equilibrium shells against radial perturbations.
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gr-qc 1years
2025 1verdicts
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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.