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.
Cosmic Shells
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abstract
When a potential for a scalar field has two local minima there arise spherical shell-type solutions of the classical field equations due to gravitational attraction. We establish such solutions numerically in a space which is asymptotically de Sitter. It generically arises when the energy scale characterizing the scalar field potential is much less than the Planck scale. It is shown that the mirror image of the shell appears in the other half of the Penrose diagram. The configuration is smooth everywhere with no physical singularity.
fields
gr-qc 1years
2025 1verdicts
UNVERDICTED 1representative citing papers
citing papers explorer
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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.